The universe demonstrates a level of fine-tuning that is absolutely astonishing. As a matter is a mere happenstance, it is extremely implausible. The conditions under which any life may exist in the universe requires extreme precision. The conditions under which intelligence physical life may exist in the universe requires even more precision. Here, I detail the fine-tuning factors for intelligent life in the universe as compiled by astronomer, Hugh Ross, in his monumental work, Why the Universe Is the Way It Is. The list of fine-tuning factors for life in general in the universe is actually longer (too long, in fact) and is housed in another blog post.
These are the factors of the fine-tuning of the galaxy, sun, earth, moon, and their combined system in supporting life. Hugh Ross has identified six different clusters of environmental necessities:
- for unicellular, low metabolism life that persists for only a brief time period
- for unicellular, low metabolism life that persists for a long time period
- for unicellular, high metabolism life that persists for a brief time period
- for unicellular, high metabolism life that persists for a long time period
- for advanced life that survives for just a brief time period
- for advanced life that survives for a long time period
From these six clusters of environmental necessities, Dr. Ross has detailed this extensive list of finely-tuned conditions for intelligent physical life:
1) galaxy cluster type
a) if too rich: galaxy collisions and mergers would disrupt solar orbit.
b) if too sparse: insufficient infusion of gas to sustain star formation for a long enough time.
2) galaxy size
a) if too large: infusion of gas and stars would disturb sun’s orbit and ignite too many galactic eruptions.
b) if too small: insufficient infusion of gas to sustain star formation for long enough time.
3) galaxy type
a) if too elliptical: star formation would cease before sufficient heavy element build-up for life chemistry.
b) if too irregular: radiation exposure on occasion would be too severe and heavy elements for life chemistry would not be available.
4) galaxy mass distribution
a) if too much in the central bulge: life-supportable planet will be exposed to too much radiation.
b) if too much in the spiral arms: life-supportable planet will be destabilized by the gravity and radiation from adjacent spiral arms.
5) galaxy location
a) if too close to a rich galaxy cluster: galaxy would be gravitationally disrupted if too close to very large galaxy(ies): galaxy would be gravitationally disrupted.
b) if too far away from dwarf galaxies: insufficient infall of gas and dust to sustain ongoing star formation
6) decay rate of cold dark matter particles
a) if too small: too few dwarf spheroidal galaxies will form which prevents star formation from lasting long enough in large galaxies so that life-supportable planets become possible.
b) if too great: too many dwarf spheroidal galaxies will form which will make the orbits of solar- type stars unstable over long time periods and lead to the generation of deadly radiation episodes.
7) hypernovae eruptions
a) if too few not enough heavy element ashes present for the formation of rocky planets.
b) if too many: relative abundances of heavy elements on rocky planets would be inappropriate for life; too many collision events in planetary system
c) if too soon: leads to a galaxy evolution history that would disturb the possibility of advanced life; not enough heavy element ashes present for the formation of rocky planets.
d) if too late: leads to a galaxy evolution history that would disturb the possibility of advanced life; relative abundances of heavy elements on rocky planets would be inappropriate for life; too many collision events in planetary system
8) supernovae eruptions
a) if too close: life on the planet would be exterminated by radiation
b) if too far: not enough heavy element ashes would exist for the formation of rocky planets.
c) if too infrequent: not enough heavy element ashes present for the formation of rocky planets.
d) if too frequent: life on the planet would be exterminated.
e) if too soon: heavy element ashes would be too dispersed for the formation of rocky planets at an early enough time in cosmic history
f) if too late: life on the planet would be exterminated by radiation.
9) white dwarf binaries
a) if too few: insufficient flourine would be produced for life chemistry to proceed.
b) if too many: planetary orbits disrupted by stellar density; life on planet would be exterminated.
c) if too soon: not enough heavy elements would be made for efficient flourine production.
d) if too late: flourine would be made too late for incorporation in protoplanet.
10) proximity of solar nebula to a supernova eruption
a) if farther: insufficient heavy elements for life would be absorbed.
b) if closer: nebula would be blown apart.
11) timing of solar nebula formation relative to supernova eruption
a) if earlier: nebula would be blown apart.
b) if later: nebula would not absorb enough heavy elements.
12) number of stars in parent star birth aggregate
a) if too few: insufficient input of certain heavy elements into the solar nebula.
b) if too many: planetary orbits will be too radically disturbed.
13) star formation history in parent star vicinity
a) if too much too soon: planetary orbits will be too radically disturbed.
14) birth date of the star-planetary system
a) if too early: quantity of heavy elements will be too low for large rocky planets to form.
b) if too late: star would not yet have reached stable burning phase; ratio of potassium-40, ura- nium-235 & 238, and thorium-232 to iron will be too low for long-lived plate tectonics to be sustained on a rocky planet.
15) parent star distance from center of galaxy
a) if farther: quantity of heavy elements would be insufficient to make rocky planets; wrong abundances of silicon, sulfur, and magnesium relative to iron for appropriate planet core characteristics.
b) if closer: galactic radiation would be too great; stellar density would disturb planetary orbits; wrong abundances of silicon, sulfur, and magnesium relative to iron for appropriate planet core characteristics.
16) parent star distance from closest spiral arm
a) if too large: exposure to harmful radiation from galactic core would be too great.
17) z-axis heights of star’s orbit
a) if more than one: tidal interactions would disrupt planetary orbit of life support planet
b) if less than one: heat produced would be insufficient for life.
18) quantity of galactic dust
a) if too small: star and planet formation rate is inadequate; star and planet formation occurs too late; too much exposure to stellar ultraviolet radiation.
b) if too large: blocked view of the Galaxy and of objects beyond the Galaxy; star and planet formation occurs too soon and at too high of a rate; too many collisions and orbit perturbations in the Galaxy and in the planetary system.
19) number of stars in the planetary system
a) if more than one: tidal interactions would disrupt planetary orbit of life support planet
b) if less than one: heat produced would be insufficient for life.
20) parent star age
a) if older: luminosity of star would change too quickly.
b) if younger: luminosity of star would change too quickly.
21) parent star mass
a) if greater: luminosity of star would change too quickly; star would burn too rapidly.
b) if less: range of planet distances for life would be too narrow; tidal forces would disrupt the life planet’s rotational period; uv radiation would be inadequate for plants to make sugars and oxygen.
22) parent star metallicity
a) if too small: insufficient heavy elements for life chemistry would exist.
b) if too large: radioactivity would be too intense for life; life would be poisoned by heavy element concentrations.
23) parent star color
a) if redder: photosynthetic response would be insufficient.
b) if bluer: photosynthetic response would be insufficient.
24) galactic tides
a) if too weak: too low of a comet ejection rate from giant planet region.
b) if too strong too high of a comet ejection rate from giant planet region.
25) H3+ production
a) if too small: simple molecules essential to planet formation and life chemistry will not form.
b) if too large: planets will form at wrong time and place for life.
26) flux of cosmic ray protons
a) if too small: inadequate cloud formation in planet’s troposphere.
b) if too large: too much cloud formation in planet’s troposphere.
27) solar wind
a) if too weak: too many cosmic ray protons reach planet’s troposphere causing too much cloud formation.
b) if too strong: too few cosmic ray protons reach planet’s troposphere causing too little cloud formation.
28) parent star luminosity relative to speciation
a) if increases too soon: runaway green house effect would develop.
b) if increases too late: runaway glaciation would develop.
29) surface gravity (escape velocity)
a) if stronger: planet’s atmosphere would retain too much ammonia and methane.
b) if weaker: planet’s atmosphere would lose too much water.
30) distance from parent star
a) if farther: planet would be too cool for a stable water cycle.
b) if closer: planet would be too warm for a stable water cycle.
31) inclination of orbit
a) if too great: temperature differences on the planet would be too extreme.
32) orbital eccentricity
a) if too great: seasonal temperature differences would be too extreme.
33) axial tilt
a) if greater: surface temperature differences would be too great.
b) if less: surface temperature differences would be too great.
34) rate of change of axial tilt
a) if greater: climatic changes would be too extreme; surface temperature differences would become too extreme.
35) rotation period
a) if longer: diurnal temperature differences would be too great.
b) if shorter: atmospheric wind velocities would be too great.
36) rate of change in rotation period
a) if longer:surface temperature range necessary for life would not be sustained.
b) if shorter:surface temperature range necessary for life would not be sustained.
37) planet age
a) if too young: planet would rotate too rapidly.
b) if too old: planet would rotate too slowly.
38) magnetic field
a) if stronger: electromagnetic storms would be too severe; too few cosmic ray protons would reach planet’s troposphere which would inhibit adequate cloud formation.
b) if weaker: ozone shield would be inadequately protected from hard stellar and solar radiation; time between magnetic reversals would be too brief for the long term maintenance of advanced life civilization
39) thickness of crust
a) if thicker: too much oxygen would be transferred from the atmosphere to the crust.
b) if thinner: volcanic and tectonic activity would be too great.
40) albedo (ratio of reflected light to total amount falling on surface)
a) if greater: runaway glaciation would develop.
b) if less: runaway greenhouse effect would develop.
41) asteroidal and cometary collision rate
a) if greater: too many species would become extinct.
b) if less: crust would be too depleted of materials essential for life.
42) mass of body colliding with primordial Earth
a) if smaller: Earth’s atmosphere would be too thick; moon would be too small.
b) if greater: Earth’s orbit and form would be too greatly disturbed.
43) timing of body colliding with primordial Earth.
a) if earlier: Earth’s atmosphere would be too thick; moon would be too small.
b) if later: sun would be too luminous at epoch for advanced life.
44) collision location of body colliding with primordial Earth
a) if too close to grazing: insufficient debris to form large moon; inadequate annihilation of Earth’s primordial atmosphere; inadequate transfer of heavy elements to Earth.
b) if too close to dead center: damage from collision would be too destructive for future life to survive.
45) oxygen to nitrogen ratio in atmosphere
a) if larger: advanced life functions would proceed too quickly.
b) if smaller: advanced life functions would proceed too slowly.
46) carbon dioxide level in atmosphere
a) if greater: runaway greenhouse effect would develop.
b) if less: plants would be unable to maintain efficient photosynthesis.
47) water vapor level in atmosphere
a) if greater: runaway greenhouse effect would develop.
b) if less: rainfall would be too meager for advanced life on the land.
48) atmospheric electric discharge rate
a) if greater: too much fire destruction would occur.
b) if less: too little nitrogen would be fixed in the atmosphere.
49) ozone level in atmosphere
a) if greater: surface temperatures would be too low.
b) if less: surface temperatures would be too high; there would be too much UV radiation at the surface.
50) oxygen quantity in atmosphere
a) if greater: plants and hydrocarbons would burn up too easily.
b) if less: advanced animals would have too little to breathe.
51) 5 nitrogen quantity in atmosphere
a) if greater: too much buffering of oxygen for advanced animal respiration; too much nitrogen fixation for support of diverse plant species.
b) if less: too little buffering of oxygen for advanced animal respiration; too little nitrogen fixation for support of diverse plant species.
52) ratio of 40K, 235,238U, 232Th to iron for the planet
a) if too low: inadequate levels of plate tectonic and volcanic activity.
b) if too high: radiation, earthquakes, and volcanoes at levels too high for advanced life.
53) rate of interior heat loss
a) if too low: inadequate energy to drive the required levels of plate tectonic and volcanic activity.
b) if too high: plate tectonic and volcanic activity shuts down too quickly.
54) seismic activity
a) if greater: too many life-forms would be destroyed; continents would grow to too large a size; vertical relief on the continents would be inadequate for the proper distribution of rain- fall, snow pack, and erosion
b) if less: nutrients on ocean floors from river runoff would not be recycled to continents through tectonics; not enough carbon dioxide would be released from carbonates; continents would not grow to a large enough size; vertical relief on the continents would become too great
55) volcanic activity
a) if lower: insufficient amounts of carbon dioxide and water vapor would be returned to the atmosphere; soil mineralization would become too degraded for life.
b) if higher: advanced life, at least, would be destroyed.
56) rate of decline in tectonic activity
a) if slower: advanced life can never survive on the planet.
b) if faster: advanced life can never survive on the planet.
57) rate of decline in volcanic activity
a) if slower: advanced life can never survive on the planet.
b) if faster: advanced life can never survive on the planet.
58) timing of birth of continent formation
a) if too early: silicate-carbonate cycle would be destabilized.
b) if too late: silicate-carbonate cycle would be destabilized.
59) oceans-to-continents ratio
a) if greater: diversity and complexity of life-forms would be limited.
b) if smaller: diversity and complexity of life-forms would be limited.
60) rate of change in oceans-to-continents ratio
a) if smaller: advanced life will lack the needed land mass area.
b) if greater: advanced life would be destroyed by the radical changes.
61) global distribution of continents (for Earth)
a) if too much in the southern hemisphere: seasonal differences would be too severe for advanced life.
62) frequency and extent of ice ages
a) if smaller: insufficient fertile, wide, and well-watered valleys produced for diverse and advanced life forms; insufficient mineral concentrations exposed for diverse and advanced life; insufficient production of high quality harbors for advanced life
b) if greater: planet inevitably experiences runaway freezing.
63) soil mineralization
a) if too nutrient poor: diversity and complexity of life-forms would be limited.
b) if too nutrient rich: diversity and complexity of life-forms would be limited.
64) gravitational interaction with a moon
a) if greater: tidal effects on the oceans, atmosphere, and rotational period would be too severe.
b) if less: orbital obliquity changes would cause climatic instabilities; movement of nutrients and life from the oceans to the continents and vice versa would be insufficient; magnetic field would be too weak.
65) Jupiter distance
a) if greater: too many asteroid and comet collisions would occur on Earth.
b) if less: Earth’s orbit would become unstable.; Jupiter’s presence would too radically disturb or
66) Jupiter mass prevent the formation of Earth
a) if greater: Earth’s orbit would become unstable; Jupiter’s presence would too radically disturb or prevent the formation of Earth
b) if less: too many asteroid and comet collisions would occur on Earth.
67) drift in major planet distances
a) if greater: Earth’s orbit would become unstable.
b) if less: too many asteroid and comet collisions would occur on Earth.
68) major planet eccentricities
a) if greater: orbit of life supportable planet would be pulled out of life support zone.
69) major planet orbital instabilities
a) if greater: orbit of life supportable planet would be pulled out of life support zone.
70) mass of Neptune
a) if too small: not enough Kuiper Belt Objects (asteroids beyond Neptune) would be scattered out of the solar system.
b) if too large: chaotic resonances among the gas giant planets would occur.
71) Kuiper Belt of asteroids (beyond Neptune)
a) if not massive enough: Neptune’s orbit remains too eccentric which destabilizes the orbits of other solar system planets.
b) if too massive: too many chaotic resonances and collisions would occur in the solar system.
72) separation distances among inner terrestrial planets
a) if too small: orbits of all inner planets will become unstable in less than 100,000,000 million years.
b) if too large: orbits of the most distant from star inner planets will become chaotic.
73) atmospheric pressure
a) if too small: liquid water will evaporate too easily and condense too infrequently; weather and climate variation would be too extreme; lungs will not function.
b) if too large: liquid water will not evaporate easily enough for land life; insufficient sunlight reaches planetary surface; insufficient UV radiation reaches planetary surface; insufficient climate and weather variation; lungs will not function.
74) atmospheric transparency
a) if smaller: insufficient range of wavelengths of solar radiation reaches planetary surface
b) if greater: too broad a range of wavelengths of solar radiation reaches planetary surface.
75) magnitude and duration of sunspot cycle
a) if smaller or shorter: insufficient variation in climate and weather.
b) if greater or longer: variation in climate and weather would be too much.
76) continental relief
a) if smaller: insufficient variation in climate and weather.
b) if greater: variation in climate and weather would be too much.
77) chlorine quantity in atmosphere
a) if smaller: erosion rates, acidity of rivers, lakes, and soils, and certain metabolic rates would be insufficient for most life forms.
b) if greater: erosion rates, acidity of rivers, lakes, and soils, and certain metabolic rates would be too high for most life forms.
78) iron quantity in oceans and soils
a) if smaller: quantity and diversity of life would be too limited for support of advanced life;
b) if very small, no life would be possible.
c) if larger: iron poisoning of at least advanced life would result.
79) tropospheric ozone quantity
a) if smaller: insufficient cleansing of biochemical smogs would result.
b) if larger: respiratory failure of advanced animals, reduced crop yields, and destruction of ozone-sensitive species would result.
80) stratospheric ozone quantity
a) if smaller: too much UV radiation reaches planet’s surface causing skin cancers and reduced plant growth.
b) if larger: too little UV radiation reaches planet’s surface causing reduced plant growth and insufficient vitamin production for animals.
81) mesospheric ozone quantity
a) if smaller: circulation and chemistry of mesospheric gases so disturbed as to upset relative abundances of life essential gases in low atmosphere.
b) if greater: circulation and chemistry of mesospheric gases so disturbed as to upset relative abundances of life essential gases in lower atmosphere.
82) quantity and extent of forest fires
a) if smaller: growth inhibitors in the soils would accumulate; soil nitrification would be insufficient; insufficient charcoal production for adequate soil water retention and absorption of certain growth inhibitors; inadequate coverage of the planet by grasslands and savannah
b) if greater: too many plant and animal life forms would be destroyed; too many forests will be converted to savannah and grassland; less carbon dioxide will be removed from the atmosphere resulting in global warming; less rainfall
83) quantity and extent of grass fires
a) if smaller: growth inhibitors in the soils would accumulate; soil nitrification would be insufficient; insufficient charcoal production for adequate soil water retention and absorption of certain growth inhibitors.
b) if greater: too many plant and animal life forms would be destroyed; too many savannahs and grasslands will be converted to deserts; less rainfall
84) quantity of soil sulfur
a) if smaller: plants will become deficient in certain proteins and die.
b) if larger: plants will die from sulfur toxins; acidity of water and soil will become too great for life; nitrogen cycles will be disturbed.
85) biomass to comet infall ratio
a) if smaller: greenhouse gases accumulate, triggering runaway surface temperature increase.
b) if larger: greenhouse gases decline, triggering a runaway freezing.
86) density of quasars if smaller: insufficient production and ejection of cosmic dust into the intergalactic medium; ongoing star formation impeded; deadly radiation unblocked. if larger: too much cosmic dust forms; too many stars form too late disrupting the formation of a solar-type star at the right time and under the right conditions for life.
87) density of giant galaxies in the early universe if smaller: insufficient metals ejected into the intergalactic medium depriving future genera- tions of stars of the metal abundances necessary for a life-support planet at the right time in cosmic history. if larger: too large a quantity of metals ejected into the intergalactic medium providing future stars with too high of a metallicity for a life-support planet at the right time in cosmic history.
88) giant star density in galaxy
a) if smaller: insufficient production of galactic dust; ongoing star formation impeded; deadly radiation unblocked.
b) if larger: too much galactic dust forms; too many stars form too early disrupting the formation of a solar-type star at the right time and under the right conditions for life.
89) rate of sedimentary loading at crustal subduction zones:
a) if smaller: too few instabilities to trigger the movement of crustal plates into the mantle thereby disrupting carbonate-silicate cycle.
b) if larger: too many instabilities triggering too many crustal plates to move down into the mantle thereby disrupting carbonate-silicate cycle
90) poleward heat transport in planet’s atmosphere
a) if smaller: disruption of climates and ecosystems; lowered biomass and species diversity; decreased storm activity and precipitation.
b) if larger: disruption of climates and ecosystems; lowered biomass and species diversity; in- creased storm activity.
91) polycyclic aromatic hydrocarbon abundance in solar nebula if smaller: insufficient early production of asteroids which would prevent a planet like Earth from receiving adequate delivery of heavy elements and carbonaceous material for life, advanced life in particular. if larger: early production of asteroids would be too great resulting in too many collision events striking a planet arising out of the nebula that could support life
92) phosphorus and iron absorption by banded iron formations
a) if smaller: overproduction of cyanobacteria would have consumed too much carbon dioxide and released too much oxygen into Earth’s atmosphere thereby overcompensating for the increase in the Sun’s luminosity (too much reduction in atmospheric greenhouse efficiency).
b) if larger: underproduction of cyanobacteria would have consumed too little carbon dioxide and released too little oxygen into Earth’s atmosphere thereby undercompensating for the increase in the Sun’s luminosity (too little reduction in atmospheric greenhouse efficiency).
93) silicate dust annealing by nebular shocks
a) if too little: rocky planets with efficient plate tectonics cannot form.
b) if too much: too many collisions in planetary system.; too severe orbital instabilities in planetary system.
94) size of galactic central bulge
a) if smaller: inadequate production of life-essential heavy elements; inadequate infusion of gas and dust into the spiral arms preventing solar type stars from forming at the right locations late enough in the galaxy’s history
b) if larger: radiation from the bulge region would kill life on the life-support planet.
95) total mass of Kuiper Belt asteroids
a) if smaller: Neptune’s orbit would not be adequately circularized.
b) if larger: too severe gravitational instabilities generated in outer solar system.
96) solar magnetic activity level
a) if greater: solar luminosity fluctuations will be too large.
97) number of hypernovae
a) if smaller: too little nitrogen is produced in the early universe, thus, cannot get the kinds of stars and planets later in the universe that are necessary for life.
b) if larger: too much nitrogen is produced in the early universe, thus, cannot get the kinds of stars and planets later in the universe that are necessary for life.
98) timing of hypernovae production
a) if too early: galaxies become too metal rich too quickly to make stars and planets suitable for life support at the right time.
b) if too late: insufficient metals available to make quickly enough stars and planets suitable for life support.
99) masses of stars that become hypernovae
a) if not massive enough: insufficient metals are ejected into the interstellar medium; that is, not enough metals are available for future star generations to make stars and planets suitable for the support of life.
b) if too massive: all the metals produced by the hypernova eruptions collapse into the black holes resulting from the eruptions; that is, none of the metals are available for future generations of stars.
100) quantity of geobacteraceae
a) if smaller or non-existent: polycyclic aromatic hydrocarbons accumulate in the surface environment thereby contaminating the environment for other life forms.
101) density of brown dwarfs
a) if too low: too many low mass stars are produced which will disrupt planetary orbits
b) if too high: disruption of planetary orbits
102) quantity of aerobic photoheterotrophic bacteria if smaller: inadequate recycling of both organic and inorganic carbon in the oceans
103) average rainfall precipitation
a) if too small: inadequate water supplies for land-based life; inadequate erosion of land masses to sustain the carbonate-silicate cycle.; inadequate erosion to sustain certain species of ocean life that are vital for the existence of all life.
b) if too large: too much erosion of land masses which upsets the carbonate-silicate cycle and has- tens the extinction of many species of life that are vital for the existence of all life.
104) variation and timing of average rainfall precipitation
a) if too small or at the wrong time: erosion rates that upset the carbonate-silicate cycle and fail to adjust adequately the planet’s atmosphere for the increase in the sun’s luminosity.
b) if too large or at the wrong time: erosion rates that upset the carbonate-silicate cycle and fail to adjust the planet’s atmosphere for the increase in the sun’s luminosity
105) average slope or relief of the continental land masses
a) if too small: inadequate erosion.
b) if too large: too much erosion.
106) distance from nearest black hole
a) if too close: radiation will prove deadly for life
107) absorption rate of planets and planetismals by parent star
a) if too low: disturbs sun’s luminosity and stability of sun’s long term luminosity.
b) if too high: disturbs orbits of inner solar system planets; disturbs sun’s luminosity and stability of sun’s long term luminosity.
108) water absorption capacity of planet’s lower mantle
a) if too low: too much water on planet’s surface; no continental land masses; too little plate tectonic activity; carbonate-silicate cycle disrupted.
b) if too high: too little water on planet’s surface; too little plate tectonic activity; carbonate-silicate cycle disrupted.
109) gas dispersal rate by companion stars, shock waves, and molecular cloud expansion in the Sun’s birthing star cluster
a) if too low: too many stars form in Sun’s vicinity which will disturb planetary orbits and pose a radiation problem; too much gas and dust in solar system’s vicinity.
b) if too high: not enough gas and dust condensation for the Sun and its planets to form; insufficient gas and dust in solar system’s vicinity.
110) decay rate of cold dark matter particles
a) if too low: insufficient production of dwarf spheroidal galaxies which will limit the maintenance of long-lived large spiral galaxies.
b) if too high: too many dwarf spheroidal galaxies produced which will cause spiral galaxies to be too unstable.
111) ratio of inner dark halo mass to stellar mass for galaxy
a) if too low: corotation distance is too close to the center of the galaxy which exposes the life-support planet to too much radiation and too many gravitational disturbances.
b) if too high: corotation distance is too far from the center of the galaxy where the abundance of heavy elements is too sparse to make rocky planets.
112) star rotation rate
a) if too slow: too weak of a magnetic field resulting in not enough protection from cosmic rays for the life-support planet.
b) if too fast: too much chromospheric emission causing radiation problems for the life-support planet.
113) rate of nearby gamma ray bursts
a) if too low: insufficient mass extinctions of life to create new habitats for more advanced species
b) if too high: too many mass extinctions of life for the maintenance of long-lived species
114) aerosol particle density emitted from forests
a) if too low: too little cloud condensation which reduces rainfall, lowers the albedo (planetary reflectivity), and disturbs climates on a global scale.
b) if too high: too much cloud condensation which increases rainfall, raises the albedo (planetary reflectivity), and disturbs climate on a global scale; too much smog.
115) density of interstellar and interplanetary dust particles in vicinity of life-support planet
a) if too low: inadequate delivery of life-essential materials
b) if too high: disturbs climate too radically on life-support planet
116) thickness of mid-mantle boundary
a) if too thin: mantle convection eddies become too strong; tectonic activity and silicate production become too great.
b) if too thick: mantle convection eddies become too weak; tectonic activity and silicate production become too small.
117) galaxy cluster density
a) if too low: insufficient infall of gas, dust, and dwarf galaxies into a large galaxy that eventually could form a life-supportable planet.
b) if too high: gravitational influences from nearby galaxies will disturb orbit of the star that has a life-supprtable planet thereby exposing that planet either to deadly radiation or to gravitational disturbances from other stars in that galaxy.
118) star formation rate in solar neighborhood during past 4 billion years
a) if too high: life on Earth will be exposed to deadly radiation or orbit of Earth will be disturbed.
119) variation in star formation rate in solar neighborhood during past 4 billion years
a) if too high: life on Earth will be exposed to deadly radiation or orbit of Earth will be disturbed.
120) gamma-ray burst events:
a) if too few: not enough production of copper, scandium, titanium, and zinc
b) if too many: too many mass extinction events
121) cosmic ray luminosity of Milky Way Galaxy:
a) if too low: not enough production of boron
b) if too high: life spans for advanced life too short; too much destruction of planet’s ozone layer
122) air turbulence in troposphere:
a) if too low: inadequate formation of water droplets
b) if too great: rainfall distribution will be too uneven
123) primordial cosmic superwinds:
a) if too low of an intensity: inadequate star formation late in cosmic history
b) if too great of an intensity: inadequate star formation early in cosmic history
124) smoking quasars:
a) if too few: inadequate primordial dust production for stimulating future star formation
b) if too many: early star formation will be too vigorous resulting in too few stars and planets being able to form late in cosmic history
125) quantity of phytoplankton:
a) if too low; inadequate production of molecular oxygen and inadequate production of maritime sulfate aerosols (cloud condensation nuclei); inadequate consumption of carbon dioxide
b) if too great: too much cooling of sea surface waters and possibly too much reduction of ozone quantity in lower stratosphere; too much consumption of carbon dioxide
126) quantity of iodocarbon-emitting marine organisms:
a) if too low: inadequate marine cloud cover; inadequate water cycling if too great: too much marine cloud cover; too much cooling of Earth’s surface
127) mantle plume production:
a) if too low: inadequate volcanic and island production rate
b) if too great: too much destruction and atmospheric disturbance from volcanic eruptions
128) quantity of magnetars (proto-neutron stars with very strong magnetic fields):
a) if too few during galaxy’s history: inadequate quantities of r-process elements are synthesized
b) if too many during galaxy’s history: too great a quantity of r-process elements are synthesized; too great of a high-energy cosmic ray production
129) frequency of gamma ray bursts in galaxy
a) if too low: inadequate production of copper, titanium, and zinc; insufficient hemisphere-wide mass extinction events
b) if too great: too much production of copper and zinc; too many hemisphere-wide mass extinction events
130) parent star magnetic field
a) if too low: solar wind and solar magnetosphere will not be adequate to thwart a significant amount of cosmic rays
b) if too great: too high of an x-ray flux will be generated
131) amount of outward migration of Neptune
a) if too low: total mass of Kuiper Belt objects will be too great; Kuiper Belt will be too close to the sun; Neptune’s orbit will not be circular enough and distant enough to guarantee long-term stability of inner solar system planets’ orbits
b) if too great: Kuiper Belt will be too distant and contain too little mass to play any significant role in contributing volatiles to life-support planet or to contributing to mass extinction events; Neptune will be too distant to play a role in contributing to the long-term stability of inner solar system planets’ orbits
132) Q-value (rigidity) of Earth during its early history
a) if too low: final obliquity of Earth becomes too high; rotational braking of Earth too low
b) if too great: final obliquity of Earth becomes too low; rotational braking of Earth is too great
133) parent star distance from galaxy’s corotation circle
a) if too close: a strong mean motion resonance will destabilize the parent star’s galactic orbit
b) if too far: planetary system will experience too many crossings of the spiral arms
134) average quantity of gas infused into the universe’s first star clusters
a) if too small: wind form supergiant stars in the clusters will blow the clusters apart which in turn will prevent or seriously delay the formation of galaxies
b) if too large: early star formation, black hole production, and galaxy formation will be too vigorous for spiral galaxies to persist long enough for the right kinds of stars and planets to form so that life will be possible
135) frequency of late impacts by large asteroids and comets
a) if too low: too few mass extinction events; inadequate rich ore deposits of ferrous and heavy metals
b) if too many: too many mass extinction events; too radical of disturbances of planet’s crust
136) level of supersonic turbulence in the infant universe
a) if too low: first stars will be of the wrong type and quantity to produce the necessary mix of elements, gas, and dust so that a future star and planetary system capable of supporting life will appear at the right time in cosmic history
b) if too high: first stars will be of the wrong type and quantity to produce the necessary mix of elements, gas, and dust so that a future star and planetary system capable of supporting life will appear at the right time in cosmic history
137) number density of the first metal-free stars to form in the universe
a) if too low: inadequate initial production of heavy elements and dust by these stars to foster the necessary future star formations that will lead to a possible life-support body
b) if too many: super winds blown out by these stars will prevent or seriously delay the formation of the kinds of galaxies that could possibly produce a future life-support body
138) size of the carbon sink in the deep mantle of the planet
a) if too small: carbon dioxide level in planet’s atmosphere will be too high
b) if too large: carbon dioxide level in planet’s atmosphere will be too low; biomass will be too small
139) rate of growth of central spheroid for the galaxy
a) if too small: inadequate flow of heavy elements into the spiral disk; inadequate outward drift of stars from the inner to the central portions of the spiral disk
b) if too large: inadequate spiral disk of late-born stars
140) amount of gas infalling into the central core of the galaxy
a) if too little: galaxy’s nuclear bulge becomes too large
b) if too much: galaxy’s nuclear bulge fails to become large enough
141) level of cooling of gas infalling into the central core of the galaxy
a) if too low: galaxy’s nuclear bulge becomes too large
b) if too high: galaxy’s nuclear bulge fails to become large enough
142) ratio of dual water molecules, (H2O)2, to single water molecules, H2O, in the troposphere
a) if too low: inadequate raindrop formation; inadequate rainfall
b) if too high: too uneven of a distribution of rainfall over planet’s surface
143) heavy element abundance in the intracluster medium for the early universe
a) if too low: too much star formation too early in cosmic history; no life-support body will ever form or it will form at the wrong tine and/or place
b) if too high: inadequate star formation early in cosmic history; no life-support body will ever form or it will form at the wrong tine and/or place
144) quantity of volatiles on and in Earth-sized planet in the habitable zone
a) if too low: inadequate ingredients for the support of life
b) if too high: no possibility for a means to compensate for luminosity changes in star
145) pressure of the intra-galaxy-cluster medium
a) if too low: inadequate star formation bursts in large galaxies
b) if too high: star formation burst activity in large galaxies is too aggressive, too frequent, and too early in cosmic history
146) level of spiral substructure in spiral galaxy
a) if too low: galaxy will not be old enough to sustain advanced life
b) if too high: gravitational chaos will disturb planetary system’s orbit about center of galaxy and thereby expose the planetary system to deadly radiation and/or disturbances by gas or dust clouds
147) mass of outer gas giant planet relative to inner gas giant planet
a) if greater than 50 percent: resonances will generate non-coplanar planetary orbits which will destabilize orbit of life-support planet
b) if less than 25 percent: mass of the inner gas giant planet necessary to adequately protect life-support planet from asteroidal and cometary collisions would be large enough to gravitationally disturb the orbit of the life-support planet
148) triggering of El Nino events by explosive volcanic eruptions
a) if too seldom: uneven rainfall distribution over continental land masses
b) if too frequent: uneven rainfall distribution over continental land masses; too much destruction by the volcanic events; drop in mean global surface temperature
149) time window between the peak of kerogen production and the appearance of intelligent life
a) if too short: inadequate time for geological and chemical processes to transform the kerogen into enough petroleum reserves to launch and sustain advanced civilization
b) if too long: too much of the petroleum reserves, both shallow subsurface and deep subsurface, will be broken down by bacterial activity into methane
150) time window between the production of cisterns in the planet’s crust that can effectively collect and store petroleum and natural gas and the appearance of intelligent life
a) if too short: inadequate time for collecting and storing significant amounts of petroleum and natural gas
b) if too long: too many leaks form in the cisterns which lead to the dissipation of petroleum and gas
151) efficiency of flows of silicate melt, hypersaline hydrothermal fluids, and hydrothermal vapors in the upper crust
a) if too low: inadequate crystallization and precipitation of concentrated metal ores that can be exploited by intelligent life to launch civilization and technology
b) if too high: crustal environment becomes too unstable for the maintenance of civilization
152) quantity of dust formed in the ejecta of Population III supernovae
a) if too low: number and mass range of Population II stars will not be great enough for a life-support planet to form at the right time and place in the cosmos; Population II stars will not form soon enough after the appearance of Population III stars
b) if too high: Population II star formation will occur too soon and be too aggressive for a life- support planet to form at the right time and place in the cosmos
153) quantity and proximity of gamma-ray burst events relative to emerging solar nebula
a) if too few and too far: inadequate enrichment of solar nebula with copper, titanium, and zinc
b) if too many and too close: too much enrichment of solar nebula with copper and zinc; too much destruction of solar nebula
154) heat flow through the planet’s mantle from radiometric decay in planet’s core
a) if too low: mantle will be too viscous and, thus, mantle convection will not be vigorous enough to drive plate tectonics at the precise level to compensate for changes in star’s luminosity
b) if too high: mantle will not be viscous enough and, thus, mantle convection will be too vigorous resulting in too high of a level of plate tectonic activity to perfectly compensate for changes in star’s luminosity
155) water absorption by planet’s mantle
a) if too low: mantle will be too viscous and, thus, mantle convection will not be vigorous enough to drive plate tectonics at the precise level to compensate for changes in star’s luminosity
b) if too high: mantle will not be viscous enough and, thus, mantle convection will be too vigorous resulting in too high of a level of plate tectonic activity to perfectly compensate for changes in star’s luminosity
156) quantity of mountains on land
a) if too small: not enough snow and ice to provide adequate melt water for life during the dry seasons
b) if too large: too much of the planet’s water would be trapped inside permanent snow and ice fields
157) average height of mountains on land
a) if too low: not enough snow and ice to provide adequate melt water for life during the dry seasons
b) if too high: too much of the planet’s water would be trapped inside permanent snow and ice fields
158) timing of late heavy bombardment
a) if too early: bombardment of Earth would be too intense; too much mass accretion; too severe a disruption of mantle and core; too much core growth if too late: bombardment of Earth would not be intense enough; too little oxygen would be delivered to the core; too little core growth
159) density and thickness of atmosphere
a) if too low: meteoritic bombardment would cause too much damage if too high: dust input to the atmosphere and soil would be too low; water input would be too low
160) degree of continental land mass barrier to oceans along rotation axis
a) if too low: rotation rate of planet slows down too slowly
b) if too high: rotation rate of planet slows down too quickly
161) methane emissions from living plants and plant litter
a) if too low: greenhouse gas input to atmosphere inadequate to prevent runaway freezing of planetary surface
b) if too high: greenhouse gas input to atmosphere launches a runaway evaporation of planet’s surface water
162) methane emissions from animals
a) if too low: greenhouse gas input to atmosphere inadequate to prevent runaway freezing of planetary surface
b) if too high: greenhouse gas input to atmosphere launches a runaway evaporation of planet’s surface water
163) methane emissions from fossil fuel production
a) if too low: greenhouse gas input to atmosphere inadequate to prevent runaway freezing of planetary surface
b) if too high: greenhouse gas input to atmosphere launches a runaway evaporation of planet’s surface water
164) lifetimes of methane in different atmospheric layers
a) if too short: greenhouse gas input to atmosphere inadequate to prevent runaway freezing of planetary surface
b) if too long: greenhouse gas input to atmosphere launches a runaway evaporation of planet’s surface water
165) average mass of the first (metal-free pop III) stars to form in the universe
a) if too low: inadequate initial production of heavy elements and dust by these stars to foster the necessary future star formations that will lead to a possible life-support body
b) if too high: super winds blown out by these stars will prevent or seriously delay the formation of the kinds of galaxies that could possibly produce a future life-support body
166) rate of release of biogenic bromides into the atmosphere
a) if too low: tropospheric ozone and nitrogen oxides abundances in the atmosphere will be too high for healthy land life; greenhouse effect of the atmosphere may be too high to compensate for changes in solar luminosity; too much ultraviolet radiation is blocked out causing plant growth to suffer
b) if too high: tropospheric ozone in the atmosphere will be too low to maintain a clean enough atmosphere for healthy land life; greenhouse effect of the atmosphere may be too low to compensate for changes in solar luminosity; ozone abundance in stratosphere will become too low to block out enough uv radiation to protect surface life
167) rate of decomposition of biogenic bromides in the atmosphere
a) if too low: tropospheric ozone and nitrogen oxides abundances in the atmosphere will be too high for healthy land life; greenhouse effect of the atmosphere may be too high to compensate for changes in solar luminosity
b) if too high: tropospheric ozone in the atmosphere will be too low to maintain a clean enough atmosphere for healthy land life; greenhouse effect of the atmosphere may be too low to compensate for changes in solar luminosity; ozone abundance in stratosphere will become too low to block out enough UV radiation to protect surface life
168) solar nebula exposure to stellar winds from expanding asymptotic giant branch stars
a) if too low: inadequate infusion of certain alkaline-earth elements into the solar nebula
b) if too high: solar nebula would suffer too much reduction and/or disruption
169) height of the tallest trees
a) if too low: inadequate interception and capture of water from rolling fog; inadequate buildup of soil nutrients and biodeposits; loss of quality timber for sustaining human civilization
b) if too high: inadequate tree growth efficiency; greater level of tree damage
170) diameter of ordinary dark matter halo surrounding the galaxy
a) if too small: spiral structure cannot be maintained long term; galaxy will grow too rapidly; galaxy structure will become too disturbed
b) if too large: spiral structure cannot be maintained long term; galaxy will not grow rapidly enough; galaxy structure will become too disturbed
171) mass of ordinary dark matter halo surrounding the galaxy
a) if too small: spiral structure cannot be maintained long term; galaxy will grow too rapidly; galaxy structure will become too disturbed
b) if too large: spiral structure cannot be maintained long term; galaxy will not grow rapidly enough; galaxy structure will become too disturbed
172) diameter of exotic dark matter halo surrounding the galaxy
a) if too small: spiral structure cannot be maintained long term; galaxy will grow too rapidly; galaxy structure will become too disturbed
b) if too large: spiral structure cannot be maintained long term; galaxy will not grow rapidly enough; galaxy structure will become too disturbed
173) mass of exotic dark matter halo surrounding the galaxy
a) if too small: spiral structure cannot be maintained long term; galaxy will grow too rapidly; galaxy structure will become too disturbed
b) if too large: spiral structure cannot be maintained long term; galaxy will not grow rapidly enough; galaxy structure will become too disturbed
174) density of ultra-dwarf galaxies (or supermassive globular clusters) in vicinity of the galaxy
a) if too low: spiral structure will not be adequately sustained; heavy element flow into galactic habitable zone will be inadequate; galactic structure stability will not be adequately maintained
b) if too high: galactic core will produce too much deadly radiation; too many heavy elements will be funneled into the galactic habitable zone; galactic structure stability will not be adequately maintained
175) magnitude of air movement at the boundaries of water vapor clouds in planet’s atmosphere
a) if too small: inadequate electrical charges induced into cloud droplets which limits how quickly droplets merge to form raindrops large enough to fall as precipitation
b) if too large: so much electrical charge would be induced into cloud droplets as to generate too frequent, too widespread, and too destructive rain and electrical storms
176) formation rate of molecular hydrogen on dust grain surfaces when the galaxy is young
a) if too low: too few stars will form during the early history of the galaxy which would delay the possible formation of a planetary system capable of sustaining advanced life past the narrow epoch in the galaxy’s history during which advanced life could exist
b) if too high: too many stars will form during the early history of the galaxy which would lead to the shutdown of star formation and spiral structure before the epoch during which a planetary system capable of sustaining advanced life could form
177) number of medium- or large-sized galaxies merging with the galaxy since the formation and stabilization of its thick galactic disk
a) if one or more: spiral structure and star formation history will be disturbed to a degree that would rule out the possibility of a planetary system capable of sustaining advanced life
178) intensity of far ultraviolet radiation from nearby stars when circumsolar disk was condensing into planets
a) if too weaker: Saturn, Uranus, Neptune, and Kuiper Belt would have been much more massive, too massive for advanced life on Earth to be possible
b) if too stronger: Uranus, Neptune, and the Kuiper Belt would never have formed and Saturn would have been smaller, making advanced life on Earth impossible
179) magnitude of chemical exchange occurring at the liquid core-deep mantle boundary of planet
a) if too small: inadequate flow of iron-rich material to planet’s surface at crustal hot spots for sustaining abundant nutrient rich flora
b) if too large: too much iron will be leached out of the planet’s core which will lower the duration and effectiveness of planet’s dynamo
180) amount of methane generated in upper mantle of planet
a) if too small: inadequate delivery of methane to planet’s atmosphere causing too little solar heat to be trapped by the atmosphere
b) if too large: too great a delivery of methane to planet’s atmosphere causing too much solar heat to be trapped by the atmosphere
181) amount of buildup of heavy elements in the galaxy
a) if too small: not enough heavy elements will be incorporated into the planetary system to make advanced life possible
b) if too large: too much heavy elements will be incorporated into the planetary system resulting in too many planetesimals, asteroids, and comets in the planetary system; galactic structure becomes too disturbed and/or frayed to allow for the existence of advanced life
182) timescale for the buildup of heavy elements in the galaxy
a) if too short: galactic structure becomes too disturbed and/or frayed to allow for the existence of advanced life; planetary system will be endowed with too great of a quantity of radiometric elements
b) if too long: planetary system will be endowed with too low of a quantity of radiometric elements; spiral structure either will collapse or too much spiral substructure will accrue
183) level of biogenic mixing of seafloor sediments
a) if too low: too low of a level of marine sediment oxygen which results in a too low biomass and nutrient budget for marine coastal ecosystems
184) production of organic aerosols in the atmosphere
a) if too small: depending on the particular aerosol either too little solar radiation is reflected into space or too little solar radiation is absorbed into the troposphere
i) if too large: depending on the particular aerosol either too much solar radiation is reflected into space or too much solar radiation is absorbed into the troposphere
185) lifetimes of organic aerosols in the atmosphere
a) if too short: depending on the particular aerosol either too little solar radiation is reflected into space or too little solar radiation is absorbed into the troposphere
b) if too long: depending on the particular aerosol either too much solar radiation is reflected into space or too much solar radiation is absorbed into the troposphere
186) total mass of primordial Kuiper Belt of asteroids and comets
a) if too small: inadequate outward drift of Jupiter, Saturn, Uranus, and Neptune; inadequate circularization of the orbits of Jupiter, Saturn, Uranus, and Neptune; late heavy bombardment of Earth would not be intense enough to bring about the necessary chemical transformation of Earth’s crust, mantle, and core; inadequate delivery of water and other volatiles to Earth
b) if too large: too much outward drift of Jupiter, Saturn, Uranus, and Neptune; late heavy bombardment of Earth would be too intense; too much delivery of water and other volatiles to Earth
187) average distance of primordial Kuiper Belt objects from the sun
a) if too short: inadequate outward drift of Uranus and Neptune; inadequate circularization of Uranus and Naptune’s orbits; either too much or too little outward drift of Jupiter and Saturn; timing and intensity of the late heavy bombardment could be altered so seriously as to create conditions on Earth detrimental to advanced life
b) if too long: inadequate outward drift of Jupiter and Saturn; inadequate circularization of Jupiter and Saturn’s orbit; either no late heavy bombardment or the late heavy bombardment could be altered so seriously as to create conditions on Earth detrimental to advanced life; inadequate outward drift of Uranus and Neptune; inadequate circularization of Uranus and Neptune’s orbits
188) quantity of sub-seaflour hypersaline anoxic bacteria
a) if too small: inadequate sulfate reduction and methangenesis to sustain the global chemical cycles essential for sustaining advanced life and human civilization; inadequate supply of concentrated metal ores for sustaining human civilization
b) if too large: too high of a level of sulfate reduction and methanogeneis to sustain the global chemical cycles essential for sustaining advanced life and human civilization
189) ratio of baryons in galaxies to baryons in between galaxies
a) if too small: galaxies in the universe would be too few and too small, yielding inadequate heavy elements to make advanced life possible
b) if too large: galaxies in the universe would be too large and too numerous, yielding a radiation and stellar density that would make advanced life impossible
190) ratio of baryons in galaxy clusters to baryons in between galaxy clusters
a) if too small: galaxies in the universe would be too few and too small, yielding inadequate heavy elements to make advanced life possible
b) if too large: galaxies in the universe would be too large and too numerous, yielding a radiation and stellar density that would make advanced life impossible
191) superwinds generated by primordial supermassive black holes
a) if too few or too weak: too few baryons would be evacuated from galaxies into the intergalactic medium; galaxies in the universe would be too large and too numerous, yielding a radiation and stellar density that would make advanced life impossible if too many or too strong: too many baryons would be evacuated from galaxies into the intergalactic medium; galaxies in the universe would be too few and too small, yielding inadequate heavy elements to make advanced life possible
192) mass of moon orbiting life support planet
a) if too small: inadequate ocean tides; planet’s rotation rate will not slow down fast enough to make advanced life possible; a mass lower than about a third of the Moon’s would not be adequate to stabilize the tilt of the planet’s rotation axis.
b) if too large: a mass higher than two percent of the Moon’s would destabilize the tilt of the planet’s rotation axis; ocean tides would be too great causing too much erosion and disturbing continental shelf life; planet’s rotation rate would slow down so quickly as to make advanced life impossible.
193) galaxy mass
a) if too small: starburst episodes occur too late in the history of the galaxy; galaxy would absorb too few dwarf and super-dwarf galaxies thereby failing to sustain star formation over a long enough period of time; structure of galaxy may become too distorted by gravitational encounters with nearby large and medium sized galaxies
b) if too large: starburst episodes occur too early in the history of the galaxy; galaxy would absorb too many medium-sized, dwarf, and super-dwarf galaxies making the radiation from the galaxy’s core too deadly and disturbing too radically the galaxy’s spiral structure
194) density of galaxies in the local volume around life-support galaxy
a) if too low: inadequate growth in the galaxy; inadequate buildup of heavy elements in the galaxy; star formation would be too anemic and history of star formation activity would be too short
b) if too high: galaxy would suffer catastrophic gravitational disturbances and star formation events would be too violent and too frequent; galaxy would grow too large and too quickly; astronomers’ view of the universe would be significantly blocked
195) average galaxy mass in the local volume around life-support galaxy
a) if too small: inadequate growth in the galaxy; inadequate buildup of heavy elements in the galaxy; star formation would be too anemic and history of star formation activity would be too short
b) if too large: galaxy would suffer catastrophic gravitational disturbances and star formation events would be too violent and too frequent; galaxy would grow too large and too quickly; astronomers’ view of the universe would be significantly blocked
196) rate at which the triple-alpha process (combining of three helium nuclei to make one carbon nucleus) runs inside the nuclear furnaces of stars
a) if too low: stars would not manufacture enough carbon and other heavy elements to make advanced life possible before cosmic conditions would rule out the possibility of advanced life; stars may too dim
b) if too high: stars would manufacture too much carbon and other heavy elements; stars may be too bright
197) surface level air pressure for life-support planet
a) if too small: lung operation in animals would be too inefficient, eliminating the possibility of high respiration rate animals; wind velocities would be too high and air streams too laminar, causing devastating storms and much more uneven rainfall distribution; less lift for aircraft making air transport more dangerous and costly
b) if too great: lung operation would be too inefficient, eliminating the possibility of high respiration rate animals; wind velocities would be too low, resulting in much lower rainfall on continental land masses; too much air resistance making air transport slower, more costly, and more dangerous.
198) average mass of cold dark gas-dust clouds in the galaxy
a) if too small: star formation will be too anemic and stretched out over too long of a time period; spiral arm structure will be disrupted; galaxy will not generate stars of the right mean mass, mass distribution, and metallicity distribution for advanced life
b) if too great: star formation will be too aggressive, occur too early, and be stretched out over too brief a time period; spiral arm structure will be disrupted; star density in neighborhood of life-support planetary system will be too high; galaxy will not generate stars of the right mean mass, mass distribution, and metallicity distribution for advanced life
199) number density of cold dark gas-dust clouds in the galaxy
a) if too low: star formation will be too anemic and stretched out over too long of a time period; spiral arm structure will be disrupted
b) if too high: star formation will be too aggressive, occur too early, and be stretched out over too brief a time period; spiral arm structure will be disrupted; solar neighborhood would include too many stars
200) level and frequency of ocean microseisms
a) if too low: inadequate rainfall; inadequate redistribution of continental shelf nutrients
b) if too high: storm intensities would become too great; rainfall levels would be too high; too much disturbance of the continental shelf environment and ecosystems
201) average slope of the coastline land masses
a) if too small: inadequate input of nutrients from the continents and islands to the continental shelves; energy from wave-wave interactions and from wave-shore interactions would be too low to adequately redistribute nutrients on the continental shelves; rainfall on continents would diminish and rainfall distribution patterns would be disrupted
b) if too great: erosion of continents and islands would be too great; continental shelf environments and ecosystems would be too radically disturbed; storms would become too in- tense; too much rain would fall on the coastlines and not enough on the continent interiors.
202) depth of Earth’s primordial ocean
a) if too shallow: moon-forming collider would not have ejected enough of Earth’s primordial ocean and atmosphere into interplanetary space; size and/or composition of the moon would be too radically disturbed
b) if too deep: moon-forming collider would have ejected too much of Earth’s primordial ocean and atmosphere into interplanetary space; size and/or composition of the moon would be too radically disturbed
203) rate of quartz re-precipitation on Earth
a) if too low: cycling of silicon would be so disturbed as to affect the production of free oxygen by phytoplankton and the removal of carbon dioxide from the atmosphere by the weathering of silicates
b) if too high: cycling of silicon would be so disturbed as to affect the production of free oxygen by phytoplankton and the removal of carbon dioxide from the atmosphere by the weathering of silicates
204) rate of release of cellular particles (fur fiber, dandruff, pollen, spores, bacteria, etc.) into the atmosphere
a) if too low: inadequate production of aerosol particles that are especially effective as cloud condensation nuclei thereby resulting into too little rain, hail, snow, and fog
b) if too high: too much production of aerosol particles that are especially effective as cloud condensation nuclei thereby casing too much precipitation or precipitation that is too un- evenly distributed
205) rate of release of protein and viral particles into the atmosphere
a) if too low: inadequate production of aerosol particles that are especially effective as cloud condensation nuclei thereby resulting into too little rain, hail, snow, and fog
b) if too high: too much production of aerosol particles that are especially effective as cloud condensation nuclei thereby casing too much precipitation or precipitation that is too un- evenly distributed
206) rate of leaf litter deposition upon soils
a) if too low: inadequate amounts of nutrients delivered to soils; inadequate amounts of silica delivered to soils; serious disruption of silica cycling
b) if too high: soils and the ecosystems within them become too deprived of light, oxygen, and carbon dioxide; interferes with nitrogen fixation;
207) availability of fossil fuels to humanity
a) if less: more greenhouse gases released to the atmosphere and more air pollution as people turn to burning wood instead; more global warming, much more respiratory diseases, and more deforestation
b) if much higher: fossil fuel burning would be accelerated resulting in more significant global warming and local cooling from release of particulates
208) date of star formation shutdown in the galaxy
a) if too soon: no possibility of planets forming with the mix of heavy elements to support advanced life
b) if too late: too high of a probability that a nearby supernova eruption or an encounter with a dense molecular cloud or a young bright star will prove deleterious to the life on the life-support planet
209) degree of central concentration of light-emitting ordinary matter for the life-support galaxy
a) if smaller: inadequate infusion of gas and dust into the spiral arms preventing solar type stars from forming at the right locations late enough in the galaxy’s history.
b) if larger: radiation from the bulge region would kill life on the life-support planet.
210) degree of flatness for the light-emitting ordinary matter for the life-support galaxy
a) if less: spiral structure either will collapse or become unstable
b) if more: inadequate infusion of gas and dust into the spiral arms preventing solar type stars from forming at the right locations late enough in the galaxy’s history
211) average albedo of Earth’s surface life
a) if less: would cause runaway evaporation of Earth’s frozen and liquid water
b) if more: would cause runaway freeze-up of Earth’s water vapor and liquid water
212) infall velocity of galaxy toward center of nearest grouping of galaxies
a) if smaller: inadequate gas and dust would be infused into the galaxy
b) if larger: galaxy would suffer serious gravitational distortions
213) infall velocity of galaxy toward center of nearest supercluster of galaxies
a) if smaller: inadequate gas and dust would be infused into the galaxy
b) if larger: galaxy would suffer serious gravitational distortions
214) distance that primordial supernovae dispersed elements heavier than helium
a) if smaller: potential life-support planet either will possess to much or too little of the vital- poison elements
b) if larger: potential life support planet will lack many of the elements essential for the support of advanced life
215) collision velocity of planet colliding with primordial Earth
a) if too low: insufficient amount of Earth’s atmosphere would be removed; too small of a moon would form
b) if too high: Earth would suffer too much destruction
216) photo erosion by nearby giant stars during planetary formation phase
a) if smaller: too low of a concentration of heavy elements in the planetary disk
b) if larger: too radical of a truncation of the outer part of the planetary disk and hence inadequate formation of gas giant planets that are distant from the star
217) dust extinction of that region of the spiral disk where the potential life support planet forms
a) if smaller: a high density rocky planet will not be able to form; potential life support planet would lack the necessary planetary companions
b) if larger: planetary system will be filled with too many asteroids and comets resulting in too many collision events and the delivery of too many volatiles
218) dust extinction in vicinity of life support planet at the time of the existence of advanced life
a) if too large: intelligent observers will experience a blocked view of the galaxy and the universe
219) surface density of the protoplanetary disk
a) if smaller: number of protoplanets produced would be too many; average protoplanet mass would be too small
b) if larger: number of protoplanets produced would be too few; average protoplanet mass would be too large
220) quantity of terrestrial lightning
a) if less: too small or too unstable of a charge-depleted zone would exist in the Van Allen radiation belts surrounding Earth making efficient communication satellite operation impossible; too few forest and grass fires would be generated; inadequate nitrogen fixation
b) if more: Earth’s Van Allen belts would become so weak that too much hard radiation would penetrate to Earth’s surface to the detriment of life; too many forest and grass fires would be generated
221) timing of solar system’s last crossing of a spiral arm
a) if earlier: humanity would now be too close to a spiral arm and thus would face more cosmic rays, a colder climate, a weaker ozone shield, and a high probability of an encounter with a large molecular cloud
b) if later: humanity would now be too close to a spiral arm and thus would face more cosmic rays, a colder climate, a weaker ozone shield, and a high probability of an encounter with a large molecular cloud; inadequate time for the buildup of resources provided by previous generations of advanced life
222) amount of iron-60 injected into Earth’s primordial core from a nearby type II supernova eruption
a) if less: inadequate differentiation of Earth’s interior layers which prevents any long-term support of plate tectonics and a strong magnetic field
b) if more: Earth’s plate tectonics would become too destructive; Earth’s interior structure would become inappropriate for the support of life and advanced life in particular
223) density of ultra-dwarf galaxies in the vicinity of the potential life-support galaxy
a) if smaller: inadequate rate of infusion of gas and dust into the potential life-support galaxy; long-term stable spiral structure cannot be sustained
b) if larger: too great of an infusion of gas and dust into the potential life-support galaxy; spiral structure will be disrupted
224) quantity of molecular hydrogen formed by the supernova eruptions of population III stars (the first born stars)
a) if smaller: inadequate formation of population II stars (second generation stars)
b) if larger: too many population II stars would form thereby limiting the production of population I stars (third generation stars)
225) quantity of soil sulfur
a) if smaller: inadequate nutrients for land life
b) if larger: organic matter would be too rapidly decomposed
226) level of oxidizing activity in the soil
a) if smaller: inadequate oxygenation of the soil for healthy root growth and the support of animal life in the soils; inadequate nutrients for land life
b) if larger: organic matter would be too rapidly decomposed
227) level of water soluable heavy metals in soils
a) if lower: inadequate trace element nutrients available for life, and especially for advanced life
b) if higher: catastrophic drop in soil microorganism diversity occurs
228) quantity of methanotrophic symbionts in wetlands
a) if lower: inadequate consumption and conversion of methane gas and inadequate delivery of carbon to mosses causing too much methane and carbon dioxide to be released to the atmosphere resulting in a global warming catastrophe
b) if higher: too much consumption and conversion of methane gas and too much delivery of carbon to mosses causing too little methane and carbon dioxide to be released to the atmosphere resulting in a global cooling catastrophe
229) ratio of asteroids to comets for the late heavy bombardment of Earth
a) if lower: inadequate delivery of heavy elements to Earth; too many volatiles would be delivered to Earth; melting of Earth would not be sufficient to adequately transform the interior of Earth.
b) if higher: inadequate delivery of volatiles to Earth; bombardment would be too destructive; chemical transformation of Earth’s interior would become inappropriate for the long-term support of advanced life
230) rate of destruction and dispersal of dust as a result of supernova eruptions in the potential life-support galaxy
a) if lower: density of asteroids and comets will be too high for the potential life-support planetary system resulting in too many impacts and too great a delivery of volatiles to the potential life-support planet; observers’ view of the galaxy and universe will be too heavily obscured
b) if higher: inadequate heavy element material for the formation of a potential life support planet; inadequate delivery of volatiles and heavy elements to the potential life-support planet from comets and asteroids.
231) quantity and diversity of viruses in the oceans
a) if lower: inadequate breakdown of particulate nutrients into usable forms for bacteria and microbial communities
b) if higher: too much devastation of bacteria, microorganisms, and larger life forms in the oceans
232) percent of baryons processed by the first stars (population III stars) in the vicinity of and inside the primordial Milky Way Galaxy
a) if lower: inadequate conversion of hydrogen and helium into heavy elements; inadequate production of molecular hydrogen; too few population II stars produced; buildup of metals will be inadequate and too slow.
b) if higher: too much conversion of hydrogen and helium into heavy elements; too much production of molecular hydrogen; too many population II stars produced; star formation would shut down too quickly before the buildup of metals would reach the necessary levels for life.
233) solar system’s orbital radius about the center of the Milky Way Galaxy
a) if shorter than just inside the corotation radius: solar system will pass through the spiral arms too many times during the history of life if at or very near the corotation radius: solar system will suffer a destructive mean motion resonance
b) if longer than the corotation radius: inadequate supply of heavy elements for the primordial solar system; solar system will pass through the spiral arms too many times during the history of life
234) quantity amommox bacteria (bacteria exploiting anaerobic ammonium oxidation reactions) in the oceans
a) if lower: food chain base in oxygen depleted marine environments would be driven to too low of a level
b) if higher: consumption of fixed nitrogen by these bacteria would deprive photosynthetic life of an important nutrient
235) quantity of soluble zinc in the oceans
a) if lower: too severe a limitation on the growth of nitrogen fixing marine bacteria; too severe a limitation on the growth of phytoplankton
b) if higher: zinc absorption by marine organisms would reach toxic levels
236) quantity of soluble silicon and silica in the oceans
a) if lower: too severe a limitation on the growth of marine diatoms which would remove an important food source from the food chain and an important contributor to both nitrogen fixation and marine aerosol production
b) if higher: silicon and silica absorption by certain marine organisms could reach toxic levels; diatom growth could become too predominant and thus damage the ecosystem
237) quantity of phosphorous and phosphates in the oceans
a) if lower: too severe a limitation on the growth of nitrogen fixing marine bacteria
b) if higher: growth of algae blooms could result in toxin release levels detrimental to other life forms
238) availability of light to upper layers of the oceans
a) if lower: inadequate phytoplankton growth in low iron content waters
b) if higher: phytoplankton growth in high iron content waters would become too aggressive and thus upset that part of marine ecosystem; certain phytoplankton blooms would release too many toxins that could prove deadly to other life forms
239) average cell size of marine phytoplankton
a) if smaller: inadequate volume within the cells to support or adequately drive many important cell functions
b) if larger: inadequate capacity of the cells to absorb important nutrients like iron and zinc
240) amount of summer ground foliage in the arctic
a) if smaller: lower reflectivity warms the arctic possibly leading to climate instabilities
b) if larger: higher reflectivity cools the arctic possibly leading to climate instabilities
241) proximity of emerging solar system nebula to red giant stars
a) if closer: solar system nebula would suffer too much damage from the radiation and gravitational pull of the red giant stars
b) if farther: solar system would not receive an adequate injection of fluorine.
242) number of red giant stars in close proximity to emerging solar system nebula
a) if smaller: solar system would not receive an adequate injection of fluorine.
b) if larger: solar system nebula would suffer too much damage from the radiation and gravitational pull of the red giant stars
243) masses of red giant stars in close proximity to emerging solar system nebula
a) if smaller: solar system would not receive an adequate injection of fluorine because it would take too long for these stars to attain their epoch of maximum fluorine production and ejection
b) if larger: solar system would not receive an adequate injection of fluorine because stars of such high mass produce too little fluorine.
244) proximity of emerging solar system nebula to fluorine-ejecting planetary nebulae
a) if closer: solar system would suffer too much radiation damage
b) if farther: solar system would not receive an adequate injection of fluorine.
245) number of fluorine-ejecting planetary nebulae in close proximity to emerging solar system nebula
a) if smaller: solar system would not receive an adequate injection of fluorine.
b) if larger: solar system would suffer too much radiation damage
246) methane production and release to the atmosphere by plants
a) if less: greenhouse effect in the atmosphere becomes too inefficient causing global cooling which could lead to a runaway freezing of the planet or to climatic instabilities
b) if more: greenhouse effect in the atmosphere becomes too efficient causing global warming which could lead to a runaway evaporation of the planet’s water or to climatic instabilities.
247) quantity of dissolved calcium in lakes and rivers
a) if smaller: inadequate removal of carbon dioxide from the atmosphere leading to climatic instabilities and possible runaway freezing
b) if larger: too much removal of carbon dioxide from the atmosphere leading to climatic instabilities and possible runaway evaporation of the planet’s liquid water and ice
248) quantity of suspended calcium in lakes and rivers
a) if smaller: inadequate removal of carbon dioxide from the atmosphere leading to climatic instabilities and possible runaway freezing.
b) if larger: too much removal of carbon dioxide from the atmosphere leading to climatic instabilities and possible runaway evaporation of the planet’s liquid water and ice.
249) frequency of core collapse supernovae
a) if smaller: inadequate production and distribution of certain heavy elements into the interstellar medium
b) if greater: too many mass extinction events on the life-support planet
250) level of rock melting during tectonic fault movements
a) if smaller: advanced life would be subject to larger and more frequent devastating earthquakes.
b) if larger: tectonic plate movement would become too rapid resulting in adequate continental stability
251) timing of continental growth spurts
a) if earlier: inadequate time for marine microorganisms to transform the chemical and physical conditions of Earth for the benefit of advanced life
b) if later: inadequate time for land life to transform the continental crust and soils for the benefit of advanced life
252) mass of the potential life support planet
a) if smaller: planet will retain too light of an atmosphere and too small of an atmospheric pressure; planet’s gravity will not be adequate to retain water vapor over a long period of time; pressure in planet’s mantle will be too low resulting in a loss of mantle conductivity and consequently a level of plate tectonics that is too weak
b) if greater: planet will retain too heavy of an atmosphere and too great of an atmospheric pressure; gravitational loss of low molecular weight gases from the atmosphere will be too low; tectonic activity level will be too strong and too short lived (it will die out too quickly)
253) quantity of clay production on continental land masses
a) if smaller: inadequate conditioning of soil for advanced plants; inadequate removal of carbon dioxide from the atmosphere; inadequate oxygenation of the atmosphere
b) if greater: inadequate aeration of soil for advanced plants; too much removal of carbon dioxide from the atmosphere
254) timing of advent of clay production on continental land masses
a) if earlier: reduction of Earth’s atmospheric greenhouse effect overtakes the increasing luminosity of the sun; bacteria will not have had sufficient time to transform the metals and nutrients into the forms needed by clay-producing life forms
b) if later: increasing luminosity of the sun overtakes the reduction of Earth’s atmospheric greenhouse effect; insufficient time for the clay-forming life forms and the ecosystems they support to build up the necessary biodeposits for humans and human civilization before the narrow time window for human civilization comes to an end
255) quantity of bacteriophages
a) if smaller: inadequate protection for advanced life against bacterial diseases
b) if greater: too much destruction of bacteria that are beneficial to advanced life
256) diversity of bacteriophages
a) if smaller: inadequate protection for advanced life against bacterial diseases
b) if greater: too much destruction of bacteria that are beneficial to advanced life
257) timing of potential life-support planet’s birth relative to spiral substructure formation
a) if earlier: inadequate supply of life-essential heavy elements from previous generations of stars in the galaxy
b) if later: too much radiation and/or gravitational disturbances from the development of spiral substructure (spurs, feathers, and filaments)
258) level of warping in the Milky Way Galaxy’s spiral disk
a) if smaller: the lack of any significant warp would imply that the MWG has had so few encounters with dwarf galaxies that it would not have received an adequate infusion of gas and dust to sustain a long enough history of star formation and the buildup of heavy elements to make advanced life possible
b) if greater: such warping would cause gravitational instabilities that would either pull the solar system out of its finely tuned orbit about the galactic center or expose it to deadly radiation from the galactic center or one of the adjacent spiral arms
259) date for opening of the Drake Passage (between South America and Antarctica)
a) if earlier: planet’s surface would have been cooled down prematurely relative to the gradual increasing luminosity of the sun
b) if later: planet’s surface would have been cooled down too late relative to the gradual increasing luminosity of the sun
260) frequency of gamma ray burst events in the galaxy
a) if smaller: insufficient number of the mass extinction events that pave the way for mass speciation events that perfectly compensate for the sun’s increasing luminosity and build up the biodeposits required by advanced life
b) if greater: too many mass extinction events would disrupt the necessary history of life on Earth that is necessary to properly compensate for the increasing luminosity of the sun and to buildup the biodeposits important for the support of human civilization
261) density of the galaxy
a) if lower: central bulge will not be big enough; spiral arms will lack the density to funnel adequate heavy elements out to the distance where an advanced life planet would be possible
b) if higher: dwarf galaxy merging with the galaxy will not sustain adequate star formation for a long enough period of time
262) impact energy of moon-forming collidor event
a) if lower: insufficient debris generated to form the moon
b) if higher: resultant debris disk dissipates too rapidly thereby preventing the formation of the moon
263) density of particulates in the atmosphere
a) if lower: inadequate cooling of planet’s surface; inadequate cooling of planet’s troposphere and stratosphere; disruption of rainfall patterns
b) if higher: too much cooling of planet’s surface; too much cooling of planet’s troposphere and stratosphere; disruption of rainfall patterns
264) frequency of giant volcanic eruptions
a) if lower: inadequate delivery of interior gases to the atmosphere; insufficient buildup of islands and continental land masses; insufficient buildup of surface crustal nutrients.
b) if higher: too much and too frequent destruction of life.
265) degree of suppression of dwarf galaxy formation by cosmic reionization
a) if lower: insufficient supply of dwarf galaxies for sustaining stable spiral structure and ongoing star formation in the life support galaxy
b) if higher: structure of life support galaxy will be disturbed too radically by merging and collision events with dwarf galaxies.
266) rate at which abiotic processes deplete nitrogen from the atmosphere by converting that nitrogen into ocean-deposited nitrates
a) if lower: inadequate supply of nitrates for diverse marine life to thrive
b) if higher: abundance of nitrogen in the atmosphere becomes too low to serve as an adequate buffer gas for advanced life
267) rate at which biological organisms convert nitrates in the ocean into free nitrogen that is subsequently released into the atmosphere
a) if lower: abundance of nitrogen in the atmosphere becomes too low to serve as an adequate buffer gas for advanced life
b) if higher: inadequate supply of nitrates for diverse marine life to thrive
268) silicon abundance in planetary system’s primordial nebula
a) if lower: planet formation and especially rocky planet formation will be too inefficient
b) if higher: planetary system will produce an overabundance of asteroids and comets resulting in too many volatiles being delivered to the potential life support planet and too many collision events for the potential life support planet; planetary system will produce too many or too massive planets and planetesimals causing catastrophic gravitational disturbances for the potential life support planet
269) rate of decrease of the thickness of the gas disk in the life-support galaxy
a) if lower: disk will not develop in a short enough time period the necessary concentration of heavy elements to make a life-support planet possible; disk will not develop the necessary density of gas and dust to adequately protect a potential life-support planet from the deadly radiation emanating from the core of the galaxy.
b) if higher: spiral substructure in the galaxy forms too quickly; disk becomes too thin to adequately protect a potential life-support planet from the deadly radiation emanating from the core of the galaxy.
270) level of upward stirring of ocean water by krill
a) if smaller: inadequate replenishment of inorganic nutrients that have been depleted by phytoplankton causing a serious drop in the productivity of phytoplankton and the regulation of atmospheric chemistry by phytoplankton; inadequate exchange of atmospheric car- bon dioxide with the stratified ocean interior.
b) if greater: too much carbon dioxide is removed from the atmosphere; potential for problematic algae blooms; disruption of the regulation of the atmospheric chemistry by phytoplankton
271) production and release of ammonium sulfate aerosols into the atmosphere
a) if lower: Earth’s surface becomes warmer leading to possible climatic instabilities;
b) if higher: Earth’s surface becomes colder leading to possible climatic instabilities
272) timing of the great oxygenation event
a) if earlier: inadequate filling of the great oxygen sinks would have occurred leading to probable large scale atmospheric oxygen abundance variations during the epoch of advanced life
b) if later: atmospheric oxygen levels required by advanced life would not have been available during the time window in which advanced life could exist
273) hydrogen escape from the atmosphere to outer space
a) if lower: too much methane is retained in the atmosphere resulting in a warming of the atmosphere and surface that could cause climatic instabilities and even a runaway evaporation of the planet’s liquid and frozen water
b) if higher: too little methane is retained in the atmosphere resulting in a cooling of the atmosphere and surface that could cause climatic instabilities and even a runaway freezing of the planet’s water
274) production of H3+ by the galaxy’s population III (first generation) stars
a) if lower: inadequate production of population II stars; too long of a delay in the production of population II stars
b) if higher: too aggressive production of population II stars; too short of a period over which population II stars are produced; subsequent star formation shuts down
275) production of H3+ by the galaxy’s population II (second generation) stars
a) if lower: inadequate production of population I stars or production of population I stars is spread out over too long of a time period
b) if higher: production of population I stars occurs over too short of a time period
276) intensity of ultraviolet radiation arriving from the sun at the time and shortly after life’s origin on Earth (before photosynthesis can establish a significant ozone shield)
a) if lower: synthesis of certain biochemical processes either will not proceed or will proceed too inefficiently.
b) if higher: many biological systems and organisms would be damaged beyond repair.
277) wavelength response pattern of ultraviolet radiation arriving from the sun at the time or shortly after life’s origin on Earth.
a) if longer wavelengths: synthesis of certain biochemical processes either will not proceed or will proceed too inefficiently.
b) if shorter wavelengths: many biological systems and organisms would be damaged beyond repair.
278) gas density of the local interstellar medium
a) if lower: inadequate suppression the heliosphere resulting in too little infall of dust from the Kuiper Belt and Oort Cloud and too little penetration of galactic cosmic rays which cause too little climatic cooling and too little ozone layer suppression respectively
b) if higher: too much suppression of the heliosphere resulting in more infall of dust from the Kuiper Belt and Oort Cloud and more penetration of galactic cosmic rays which cause climatic cooling and ozone layer suppression respectively
279) mass of the disk of dust, asteroids, and comets for the primordial planetary system
a) if smaller: late heavy bombardment will not be intense enough to adequately transform the interior of the potential life support planet; inadequate bombardment during life’s history to generate the extinction events to prepare the planet for advanced life
b) if greater: orbits of the planets become too chaotic
280) magnitude of tidal Coulomb stresses (stress imparted by tides on tectonic fault zones)
a) if smaller: tectonic events will become more violent
b) if greater: tides will cause too much disruption and/or destruction of continental shelf habitats and continental shelf life
281) amount of methane stored in ocean clathrates
a) if smaller: inadequate methane would be available for certain critical chemoautotrophs.
b) if greater: serious risk of one or more massive global warming events that could devastate advanced life.
282) ratio of viscous to rotational forces in the planet’s liquid core
a) if smaller: inadequate chemical and physical exchanges between the lower mantle and the core and between the inner and outer core.
b) if greater: serious disruptions in the operation of the planet’s dynamo would radically disturb or deteriorate the planet’s magnetic field and tectonics.
283) planet’s oxygenation time (time for atmospheric oxygen to reach a level capable of supporting advanced life)
a) if longer: planet’s star will no longer be stable enough to provide a steady, non-lethal illumination
b) if shorter: oxygenation either would continue rising reaching a level that would no longer support long-lived advanced animals and would lead to too many grass and forest fires or the oxygenation levels would vary too much for stable advanced life ecosystems
284) inward migration of icy rubble from the outer primordial planetary disk
a) if smaller: potential life support planet will be too dry.
b) if greater: potential life support planet either will be too wet or too water vapor laden
285) timing of the appearance of methanogenic bacteria relative to the timing of the appearance of photosynthetic bacteria
a) if earlier: causes a non-linear runaway increase of the accumulation of methane in the atmosphere which would result in a greenhouse effect that would evaporate all of the planet’s water.
b) if later: inadequate input of methane in the atmosphere to build up enough of a greenhouse effect to compensate for the fainter sun at that time.
286) relative abundance of methanogenic life compared to photosynthetic life
a) if smaller: inadequate input of methane into the atmosphere which results in too weak of a greenhouse effect thereby leading to catastrophic cooling
b) if greater: too much input of methane into the atmosphere which results in too strong of a greenhouse effect thereby leading to catastrophic heating
287) ratio of iron to chondritic meteorites at the time and place of Earth’s birth
a) if smaller: Earth will not be dense enough; Earth would not sustain a long-lived strong magnetic field and plate tectonics.
b) if greater: Earth will be too dense; Earth’s crust would be too iron-rich; Earth’s dynamo will not be stable enough
288) number of ultracompact dwarf galaxies in the vicinity of the potential life support galaxy during that galaxy’s youth
a) if lower: potential life support galaxy will not grow to a large enough size; inadequate star formation during the potential life support galaxy’s youth.
b) if higher: potential life support galaxy will grow too large; structure of the potential life support galaxy will become too distorted.
289) number of starless hydrogen gas clouds in the near vicinity of the potential life support galaxy
a) if smaller: insufficient infusion of gas into the galaxy to sustain the spiral structure and a sufficiently high level of ongoing star formation in the galaxy.
b) if greater: too much infusion of gas into the galaxy resulting in the formation of too much spiral substructure and/or too much growth in the galaxy.
290) average mass of starless hydrogen gas clouds in the near vicinity of the potential life support galaxy
a) if smaller: insufficient infusion of gas into the galaxy to sustain the spiral structure and a sufficiently high level of ongoing star formation in the galaxy.
b) if greater: too much infusion of gas into the galaxy resulting in the formation of too much spiral substructure and/or too much growth in the galaxy.
291) dust to gas ratio in and near the core of the potential life support galaxy during that galaxy’s youth
a) if smaller: insufficient production of molecular hydrogen in this region leading to an inadequate star formation rate early in the galaxy’s history.
b) if greater: too much production of molecular hydrogen in this region leading to too high of a star formation rate early in the galaxy’s history which in turn limits the later formation of population I type stars
292) dust temperature in and near the core of the potential life support galaxy during that galaxy’s youth
a) if lower than 10°K: formation of molecular hydrogen is suppressed which causes star formation in this region to cease or become severely limited
b) if higher than 500°K: formation of molecular hydrogen is suppressed which causes star formation in this region to cease or become severely limited
c) if too close to the ideal temperature for formation of molecular hydrogen: too high of a star formation rate in this region early in the galaxy’s history which limits the later formation of population I stars
d) if too far from the ideal temperature for formation of molecular hydrogen: inadequate star formation rate in this region early in the galaxy’s history
293) gas temperature in and near the core of the potential life support galaxy during that galaxy’s youth
a) if higher than a few hundred °K: formation of molecular hydrogen in this region is suppressed which causes star formation to cease or become severely limited
b) if too close to the ideal temperature for formation of molecular hydrogen: too high of a star formation rate in this region early in the galaxy’s history which limits the later formation of population I stars
c) if too far from the ideal temperature for formation of molecular hydrogen: inadequate star formation rate in this region early in the galaxy’s history
294) dust to gas ratio in the mid to outer parts of the potential life support galaxy during that galaxy’s youth
a) if smaller: insufficient production of molecular hydrogen in this region leading to an inadequate star formation rate early in the galaxy’s history.
b) if greater: too much production of molecular hydrogen in this region leading to too high of a star formation rate early in the galaxy’s history which in turn limits the later formation of population I type stars
295) dust temperature in the mid to outer parts of the potential life support galaxy during that galaxy’s youth
a) if lower than 10°K: formation of molecular hydrogen in this region is suppressed which causes star formation to cease or become severely limited.
b) if higher than 500°K: formation of molecular hydrogen in this region is suppressed which causes star formation to cease or become severely limited.
c) if too close to the ideal temperature for formation of molecular hydrogen: too high of a star formation rate in this region early in the galaxy’s history which limits the later formation of population I stars.
d) if too far from the ideal temperature for formation of molecular hydrogen: inadequate star formation rate in this region early in the galaxy’s history.
296) gas temperature in the mid to outer parts of the potential life support galaxy during that galaxy’s youth
a) if higher than a few hundred °K: formation of molecular hydrogen in this region is suppressed which causes star formation to cease or become severely limited
b) if too close to the ideal temperature for formation of molecular hydrogen: too high of a star formation rate in this region early in the galaxy’s history which limits the later formation of population I stars.
c) if too far from the ideal temperature for formation of molecular hydrogen: inadequate star formation rate in this region early in the galaxy’s history
297) quantity of carbon monoxide in the potential life support galaxy early in its history
a) if lower: inadequate cooling of the molecular gas clouds causing too few stars to form at this time.
b) if higher: too much cooling of the molecular gas clouds causing too many star to form at this time which limits how many stars can form later.
298) quantity of carbon monoxide in the potential life support galaxy late in its history.
a) if lower: inadequate cooling of the molecular gas clouds causing too few stars to form at this time.
b) if higher: too much cooling of the molecular gas clouds causing too many stars to form at this time, stars whose radiation and gravity could disrupt life on a life support planet
299) number density of dark matter minihalos in the primordial Local Group
a) if lower: galaxies in the Local Group will not grow fast enough and/or large enough
b) if higher: galaxies in the Local Group will grow too quickly and/or grow to be too large
300) intensity or speed of high-velocity galactic outflows during the youth of the potential life support galaxy
a) if lower: not enough gas and dust is ejected from the galaxy resulting in the galaxy growing to too large of a size and especially causing the galactic bulge to become too large and too massive.
b) if higher: causes star formation to terminate too quickly; too great a loss of heavy elements from the galaxy.
301) thickness of the thick disk for the potential life support galaxy
a) if thinner: spiral disk will not remain sufficiently stable, sufficiently flat, and/or sufficiently free of substructure for a long enough period of time.
b) if thicker: spiral disk will not be dense enough resulting in inadequate protection for the potential life support planet from deadly radiation emanating out from the galaxy’s central bulge.
302) rate at which the thick disk for the potential life support galaxy grows thinner
a) if faster: spiral disk will not remain sufficiently stable, sufficiently flat, and/or sufficiently free of substructure for a long enough period of time.
b) if slower: spiral disk will not be dense enough resulting in inadequate protection for the potential life support planet from deadly radiation emanating out from the galaxy’s central bulge.
303) mass of the corona surrounding the potential life support galaxy
a) if smaller: inadequate reservoir of baryons for sustaining ongoing star formation.
b) if greater: too large of reservoir of baryons for sustaining ongoing star formation resulting in a too aggressive rate of ongoing star formation.
304) diameter of the corona surrounding the potential life support galaxy
a) if smaller: reservoir of baryons in the corona will too efficiently sustain ongoing star formation in the galaxy resulting in a too aggressive rate of ongoing star formation.
b) if greater: reservoir of baryons will not sustain an efficient enough ongoing star formation rate for the galaxy.
305) average strength of local gravitational instabilities in the potential life support galaxy
a) if smaller: gas collapse is too slow and too inefficient resulting in too slow of a rate of star formation.
b) if greater: gas collapse is too quick and too efficient resulting in a too rapid rate of star formation.
306) date of the last large merging event with the potential life support galaxy
a) if earlier: inadequate growth in the galaxy; inadequate infusion of gas and dust into the galaxy; inadequate star formation later in the galaxy’s history.
b) if later: morphology of the galaxy remains too disturbed at life-critical epochs in the galaxy’s history; star formation history would be disrupted.
307) distance of the snow line from the primordial sun at the time of planet formation
a) if closer: gas giant planets will form too close to the sun; inner solar system would be too volatile rich
b) if farther: gas giant planets will form too distant from the sun; inner solar system would be volatile poor
308) distance of the tar line from the primordial sun at the time of planet formation
a) if closer: Jupiter-type planet and main belt asteroids will form too close to the sun; inner solar system bodies will be gravitationally disrupted.
b) if farther: Jupiter-type planet and main belt asteroids will form too far from the sun; Earth will not be adequately protected from comet and asteroid collisions from incoming objects from the Kuiper Belt and Oort Cloud.
309) outer radius of the “dead zone,” the low-viscosity, very-low-ionization zone for the primordial planetary disk
a) if closer: gas giant planets will form too close to the sun; inner solar system would be too gravitationally disturbed.
b) if farther: gas giant planets will form too distant from the sun; inner solar system would not be adequately protected from comet and asteroid collisions.
310) cooling efficiency of the protoplanetary disk
a) if smaller: either gas giant planets will not form or they will be too small , too few, or too distant from their star.
b) if greater: gas giant planets either will be too close to their star or too numerous or too massive.
311) outer protoplanetary disk lifetime
a) if shorter: inadequate initial inward migration of gas giant planets
b) if longer: too much initial inward migration of gas giant planets
312) solid to gas ration in the outer protoplanetary disk
a) if smaller: either gas giant planets will not form or they will be too small or too few; gas giant planet formation times will be too long.
b) if greater: gas giant planets either will be too numerous or too massive; gas giant planet formation times will be too short.
313) level of large scale turbulence in the protoplanetary disk
a) if smaller: inadequate transfer of refractory phases from the inner solar system to the outer solar system; inadequate transfer of carbonaceous materials from the interstellar medium and the outer solar system to the inner solar system.
b) if greater: too much transfer of refractory material from the inner to the outer solar system; too much transfer of carbonaceous materials from the interstellar medium and the outer solar system to the inner solar system; too much chaos introduced to the protoplanetary disk.
314) tidal stripping of low-mass dark matter halos during the early history of the Local Group of galaxies
a) if smaller: either too many dwarf galaxies would form or too many star-poor intergalactic dark matter structures would exist.
b) if greater: either not enough dwarf galaxies would form or not enough star-poor intergalactic dark matter structures would exist.
315) efficiency of gas cooling in low-mass dark matter halos during the early history of the Local Group of galaxies
a) if smaller: early star formation in Local Group dwarf galaxies would be too aggressive.
b) if greater: early star formation in Local Group dwarf galaxies would not be aggressive enough.
316) intensity of extragalactic ultraviolet radiation in the vicinity of low-mass dark matter halos during the early history of the Local Group of galaxies
a) if smaller: early star formation in Local Group dwarf galaxies would not be aggressive enough.
b) if greater: early star formation in Local Group dwarf galaxies would be too aggressive
317) average magnetic energy density in the quiet solar photosphere
a) if smaller: inadequate heating of the solar corona; inadequate solar chromospheric radiation.
b) if greater: too much heating of the solar corona; too much solar chromospheric radiation.
318) number of tectonic plates making up the surface crust
a) if fewer: too few continents and large islands; inadequate subduction; volcanism and tectonic movements either will be too little or too much.
b) if greater: too many continents and large islands; too much subduction; volcanism and tectonic movements either will be too little or too much.
319) number density of spicules on the solar surface
a) if smaller: inadequate transfer of mass into the solar corona; spectral luminosity profile of the sun would be disturbed.
b) if greater: too much transfer of mass into the solar corona; spectral luminosity profile of the sun would be disturbed.
320) proximity of the primordial solar system nebula to the remnants of eruptions of novae
a) if closer: solar system nebula would be over-enriched in silicon-carbon grains.
b) if farther: solar system nebula would be under-enriched in silicon-carbon grains.
321) supernova rate in the life support galaxy
a) if smaller: inadequate production of heavy elements.
b) if greater: cosmic ray intensity would be too great.
322) timing of the initiation of enrichment of the interstellar medium with s-process elements for the potential life-support galaxy
a) if earlier: star formation may shut down too soon; spiral structure may collapse or become too chaotic.
b) if later: inadequate supply of s-process elements would be available for the potential life- support planet.
323) proximity of the emerging solar system nebula to either a white dwarf or a neutron star that is accreting hydrogen gas or to the stellar winds blowing out from a neutron star or a collapsar disk.
a) if closer: solar system nebula will be disrupted or stripped of gas.
b) if farther: solar system nebula will fail to be adequately enriched with p-process elements that are heavier than iron.
324) density of baryons in the Local Volume of the universe
a) if smaller: galaxies would be too small and numerically too sparse
b) if greater: galaxies would be too big and too numerous
325) ratio of baryons in galaxies to baryons in between galaxies in the Local Volume of the universe
a) if smaller: galaxies would be too small and numerically too sparse.
b) if greater: galaxies would be too big and too numerous.
326) density of baryons in the Local Group of galaxies
a) if smaller: galaxies would be too small and numerically too sparse.
b) if greater: galaxies would be too big and too numerous.
327) ratio of baryons in galaxies to baryons in between galaxies in the Local Group of galaxies
a) if smaller: galaxies would be too small and numerically too sparse.
b) if greater: galaxies would be too big and too numerous.
328) epoch of peak star formation in the potential life support galaxy
a) if earlier: not enough stars form late in the galaxy’s history.
b) if later: too many stars form late in the galaxy’s history.
329) mass of the galaxy’s central black hole
a) if smaller: central bulge of the galaxy will be too small; the central bulge will be too gas rich.
b) if greater: central bulge of the galaxy will be too large; the central bulge will be too gas poor.
330) ratio of type I to type II supernovae in the potential life support galaxy
a) if smaller: will not have the right mix of heavy elements for the potential life support planet.
b) if greater: will not have the right mix of heavy elements for the potential life support planet.
331) ratio of polycyclic aromatic hydrocarbons to stars in the galaxy
a) if smaller: planet formation in the galaxy will be suppressed; too few population I stars (late- born stars) in the galaxy.
b) if greater: too many asteroids and comets will form; late history star formation will be too aggressive .
332) number density of intracluster clouds in and around the Local Group of galaxies
a) if smaller: inadequate infusion of gas and dust into the Milky Way Galaxy for sustaining sufficient rate of ongoing star formation.
b) if greater: Milky Way Galaxy and hence the solar system will be too radically disturbed.
333) average mass of intracluster clouds in and around the Local Group of galaxies.
a) if smaller: inadequate infusion of gas and dust into the Milky Way Galaxy for sustaining sufficient rate of ongoing star formation.
b) if greater: Milky Way Galaxy and hence the solar system will be too radically disturbed.
334) metallicity of the galaxy’s halo
a) if lower; inadequate infusion of metals into the galaxy’s disk.
b) if higher: too much development of spiral substructure or too much disturbance of the main spiral structure.
335) inward migration of icy meter-sized rubble from the outer part of the protoplanetary disk
a) if smaller: potential life support planet will become too dry.
b) if greater: potential life support planet will become too wet.
336) density of stars in the sun’s birthing star cluster
a) if smaller: solar system will retain too many of its primordial Oort Cloud and Kuiper Belt objects which leads to greater impact rates on Earth; solar system will not capture enough bodies from protoplanetary disks surrounding nearby stars.
b) if greater: solar system will lose too many of its primordial Oort Cloud and Kuiper Belt objects which leads to an inadequate impact rates on Earth; solar system may capture too many bodies from protoplanetary disks surrounding nearby stars.
337) carbon abundance in the protoplanetary disk of the potential life support planetary system
a) if smaller: potential life support planet will become too carbon poor.
b) if greater: potential life support planet will become too carbon rich.
338) number density of dark matter subhalos surrounding the galaxy
a) if smaller: inadequate infusion of gas and dust into the galaxy.
b) if greater: too much star formation would occur in the outer parts of the galaxy’s disk.
339) average mass of the dark matter subhalos surrounding the galaxy
a) if smaller: inadequate infusion of gas and dust into the galaxy.
b) if greater: too much star formation would occur in the outer parts of the galaxy’s disk.
340) formation times for the dark matter halo and subhales surrounding the galaxy.
a) if earlier: too many satellite galaxies and satellite gas clouds will form.
b) if later: too few satellite galaxies and satellite gas clouds will form.
341) ratio of average surface magnetic field strength to the expansion factor of open magnetic flux tubes on the sun
a) if smaller: solar wind speed will be too low; not enough suppression of Earth’s ionosphere or of ozone in the stratosphere
b) if greater: solar wind speed will be too high resulting in too many and too intense geomagnetic storms; too much suppression of Earth’s ionosphere, and too much destruction of ozone in the stratosphere
342) rate of growth of the galactic bulge in the spiral galaxy
a) if slower: buildup of heavy element abundance would take place too slowly; galaxy will be too metal poor.
b) if faster: buildup of heavy element abundance would occur too quickly; galaxy will be too metal rich; galaxy’s physical structure would probably become too disturbed.
343) strength of the ultraviolet background for the protogalaxy.
a) if weaker: protogalaxy will collapse too efficiently and too quickly; spiral structure will not form or too much star formation will occur early in the galaxy’s history.
b) if stronger: protogalaxy either will not collapse or it will collapse too slowly and too inefficiently; spiral structure will not form or too few stars will form early in the galaxy’s history.
344) proximity of the emerging solar system nebula to very low mass red giant and asymptotic giant branch stars
a) if closer: emerging solar system nebula will be exposed to too much radiation and may suffer too much gravitational disturbance.
b) if farther: emerging solar system nebula will not be adequately enriched with large-grained graphite, silicon carbide, corundum, and spinel.
345) richness or density of galaxies in the supercluster of galaxies
a) if smaller: inadequate supply of dwarf galaxies for sustaining the spiral structure and the star formation history for the potential life support galaxy.
b) if greater: density of galaxies would be so great as to disturb the structure and the star formation history of the potential life support galaxy.
346) misalignment angle between the magnetic and rotational axes of the star during the planet formation era.
a) if smaller: inadequate inward migration of the planets from their birthing sites in the proto-planetary disk.
b) if greater: too much inward migration of the planets from their birthing sites in the proto-planetary disk.
347) infall velocity of matter into the dark matter halo of the potential life support galaxy
a) if smaller: inadequate accretion of matter; inadequate accretion of satellite dark matter halos; dark matter halo remains too small.
b) if greater: too much accretion of matter; too much accretion of satellite dark matter halos; dark matter halo becomes too large.
348) quantity of hydroxyl (OH) in the planet’s troposphere
a) if smaller: too much methane and carbon monoxide would accumulate in the planet’s atmosphere resulting in a powerful greenhouse effect and respiratory problems for advanced life; too little ozone would be produced in the troposphere.
b) if greater: not enough methane would accumulate in the planet’s atmosphere; too much ozone would be produced in the troposphere.
349) quantity of hydroxyl (OH) in the planet’s stratosphere
a) if smaller: too much methane and carbon monoxide would accumulate in the planet’s atmosphere resulting in a powerful greenhouse effect and respiratory problems for advanced life; too little ozone would be produced in the stratosphere.
b) if greater: not enough methane would accumulate in the planet’s atmosphere; too much ozone would be produced in the stratosphere.
350) level of magnetization of the spiral disk for the potential life support galaxy
a) if smaller: spiral structure will lack long term stability.
b) if greater: too much spiral substructure (spurs and feathers) will develop.
351) metallicity of the galaxy’s halo
a) if smaller: inadequate infusion of heavy elements into the habitable zone of the galaxy.
b) if greater: too much disturbance of the spiral structure of the galaxy or too much growth in the galaxy’s main structure and/or substructure.
352) strength of the wind emanating from the galaxy’s nuclear core
a) if smaller: galactic bulge will grow too large; inadequate heavy element enrichment of the galaxy’s habitable zone.
b) if greater: galactic bulge will remain too small; too great a buildup of spiral substructure; too much disturbance of the galaxy’s habitable zone.
353) mass of the initial or primordial galaxy
a) if smaller: rate if merger events with other galaxies will be too low.
b) if greater: rate of merger events with other galaxies will be too high.
354) mass of the galaxy’s central black hole
a) if smaller: outflow from the vicinity of the black hole will not adequately suppress star formation in the galaxy.
b) if greater: outflow from the vicinity of the black hole will too aggressively suppress star formation in the galaxy.
355) date for the formation of the galaxy’s central black hole
a) if earlier: outflows from the vicinity of the black hole may too quickly or too aggressively suppress star formation in the galaxy.
b) if greater: outflows from the vicinity of the black hole may not adequately suppress star formation early enough or aggressively enough.
356) level of mixing of the elements and chemicals in the protoplanetary disk
a) if smaller: Earth will not have an adequate abundance of the lighter elements and compounds.
b) if greater: Earth will not possess an adequate abundance of the heaviest elements and compounds.
357) level of enhanced mixing in the interiors of low-mass red giant stars that were in the vicinity of the solar system’s protoplanetary disk
a) if smaller: inadequate infusion of flouring into the solar system’s protoplanetary disk.
b) if greater: too much infusion of fluorine into the solar system’s protosplanetary disk.
358) date when half the stars in the galaxy would have already been formed
a) if earlier: inadequate buildup of heavy elements.
b) if later: too much disruption of the galaxy’s structure and radiation late in its history.
359) density of dwarf dark matter halos in the vicinity of the Milky Way Galaxy
a) if smaller: number of small-scale merger events will be too low to maintain the Galaxy’s spiral structure and ongoing star formation history.
b) if greater: number of small-scale merger events will be too high resulting in too much growth and too much disturbance of the Galaxy.
360) metallicity enrichment by dwarf galaxies of the intergalactic medium in the vicinity of the potential life support galaxy
a) if smaller: inadequate metal enrichment of the galaxy.
b) if greater: too much metal enrichment of the galaxy.
361) average star formation rate throughout cosmic history for dwarf galaxies that are in the vicinity of the potential life support galaxy
a) if smaller: too much infusion of gas into the potential life support galaxy which results in too aggressive episodes of star formation in that galaxy during the potential life support epoch.
b) if greater: inadequate infusion of gas into the potential life support galaxy which results in too anemic episodes of star formation in that galaxy leading up to the potential life support epoch.
362) quantity of heavy elements infused into the intergalactic medium by dwarf galaxies in the vicinity of the potential life support galaxy during the first two billion years of cosmic history.
a) if smaller: inadequate metal enrichment of the galaxy.
b) if greater: too much metal enrichment of the galaxy.
363) quantity of heavy elements infused into the intergalactic medium by the superwinds of large galaxies in the vicinity of the potential life support galaxy during the first two billion years of cosmic history
a) if smaller: inadequate metal enrichment of the galaxy.
b) if greater: too much metal enrichment of the galaxy.
364) quantity of diffuse, large-grained intergalactic dust in the vicinity of the potential life support galaxy
a) if smaller: inadequate enrichment of certain heavy elements into the galaxy during its late his- tory
b) if greater: too much enrichment of certain heavy elements into the galaxy during its late history
365) ratio of baryonic matter to exotic matter in dwarf galaxies in the vicinity of the potential life support galaxy
a) if smaller: dwarf galaxies will not be stable enough and hence will be subject to early dissipation and/or destruction.
b) if greater: dwarf galaxies will cause too great of a gravitational disturbance when they are absorbed by the potential life support galaxy.
366) ratio of baryons in the intergalactic medium relative to baryons in the circumgalactic medium for the potential life support galaxy
a) if smaller: galaxy will receive too many merger events with other galaxies.
b) if greater: galaxy’s structure will not be stable for a long enough period of time.
367) intergalactic photon density in the vicinity of the potential life support galaxy
a) if smaller: optical depth of intergalactic space in the vicinity of the galaxy will be too low resulting in too much deadly radiation from gamma ray burst events and other high-energy phenomena in the universe.
b) if greater: optical depth of intergalactic space in the vicinity of the galaxy will be too high resulting in an inadequate production of certain heavy elements and inadequate seeding of the life support planet’s atmosphere.
368) frequency of mega-volcanic eruptions on the life support planet
a) if lower: inadequate replenishment of soil fertility; inadequate number of mass extinction events.
b) if higher: too much disturbance of the global climate; too many mass extinction events.
369) timing of the introduction of the equivalent of a human species relative to the last mega-volcanic eruption
a) if too soon: global climate and the ozone shield will not have had adequate time to recover.
b) if too late: too high of a risk of a subsequent mega-volcanic eruption; inadequate soil enrichment.
370) percentage of the planet’s surface covered by forests
a) if smaller: inadequate absorption of carbon dioxide from the atmosphere resulting in too much global warming; altered albedo of the planet disturbs global climate; inadequate release of aerosols to the atmosphere lowers global rainfall; inadequate habitat space for certain plant and animal species
b) if greater: too much absorption of carbon dioxide from the atmosphere resulting in too much global cooling; altered albedo of the planet disturbs global climate; too much release of aerosols to the atmosphere increases global rainfall; inadequate habitat space for certain species of plants and animals
371) high latitude precipitation
a) if lower: inadequate moisture for abundant high latitude biota.
b) if higher: too much high latitude glaciation.
372) duration of El Nino events
a) if shorter: rainfall distribution becomes too uneven.
b) if longer: rainfall distribution becomes too uneven; too much global warming.
373) quantity and diversity of plant parasites
a) if lower: inadequate nutrient cycling in the soils; reduced plant diversity.
b) if higher: too much devastation of plants.
374) quantity and diversity of fungi on the continental land masses
a) if lower: inadequate production of clays and clay sediments leading to an inadequate rate of burial of organic carbon which in turn results in too little and too late oxygenation of the planet’s atmosphere.
b) if higher: too much devastation of plants and animals.
375) quantity of volatile organic compounds released into the atmosphere by trees
a) if lower: inadequate removal of ground level and tropospheric ozone; inadequate removal of hydroxyl radicals from the troposphere; inadequate production of organic haze; inadequate production of organic aerosols.
b) if higher: too much removal of ground level and tropospheric ozone; too much removal of hydroxyl radicals from the troposphere; too much production of organic haze; too much production of organic aerosols.
376) average pore pressure at subduction zones
a) if lower: inadequate lubrication of subduction zones leads to many destructive earthquakes.
b) if higher: too much slippage will occur at subduction zones causing continental plate movements to become too rapid.
377) average rate of migration of aqueous fluids through the planet’s upper crust.
a) if lower: inadequate heavy-metal ore deposits will be generated.
b) if higher: planet’s upper crust becomes too unstable.
378) trace element abundance in atmospheric dust
a) if lower: inadequate delivery of critical nutrients to surface marine life which limits both the rate of calcification by marine life and the sequestration of carbon into the deep ocean which in turn affects the global climate.
b) if higher: delivery of critical nutrients to surface marine life leads to large algal blooms which can poison certain life forms and which increases the rate of calcification by marine life and the sequestration of carbon into the deep ocean which in turn affects the global climate
379) level of dust supply to the surfaces of oceans
a) if lower: inadequate delivery of critical nutrients to surface marine life which limits both the rate of calcification by marine life and the sequestration of carbon into the deep ocean which in turn affects the global climate
b) if higher: delivery of critical nutrients to surface marine life leads to large algal blooms which can poison certain life forms and which increases the rate of calcification by marine life and the sequestration of carbon into the deep ocean which in turn affects the global climate.
380) soil moisture level
a) if lower: inadequate precipitation upon continental land masses.
b) if higher: too much precipitation upon continental land masses.
381) level of deep ocean convection
a) if lower: inadequate oxygenation of the deep ocean; deep sea life suffers.
b) if higher: inadequate oxygen supplies for life just below the ocean surface.
382) rate of remineralization of particulate organic matter
a) if lower: export of carbon from the surface ocean to the deep ocean and the ocean floor is much reduced resulting in a buildup of carbon dioxide in the atmosphere and subsequent global warming and a possible runaway evaporation of water.
b) if higher: export of carbon from the surface ocean to the deep ocean and the ocean floor is much enhanced resulting in a reduction of carbon dioxide in the atmosphere and sub- sequent global cooling and a possible runaway freezeup.
383) quantity of large-celled sulfur bacteria in the oceans
a) if lower: inadequate deposition of phosphates and phosphorite on the sea floor thereby removing a major source of future phosphorus nutrients for land life and a major source of phosphate and phosphorite deposits for human exploitation.
b) if higher: inadequate phosphorus will be available to sustain a large biomass of surface marine life.
384) quantity of sulfuric acid in the troposphere
a) if lower: inadequate formation of cloud condensation nuclei causing less rain to fall and a significant change in the planet’s albedo.
b) if higher: acid rain negatively impacts the biosphere.
385) quantity of ammonia in the troposphere
a) if lower: inadequate formation of cloud condensation nuclei causing less rain to fall and a significant change in the planet’s albedo.
b) if higher: advanced life forms will experience respiratory problems; acid rain negatively impacts the biosphere.
386) quantity of iodine oxide in the troposphere
a) if lower: inadequate formation of cloud condensation nuclei causing less rain to fall and a significant change in the planet’s albedo.
b) if higher: certain life forms may esperie4nce toxic levels of iodine while others may suffer from a lack of iodine.
387) level of atmospheric oxidation of aromatics
a) if lower: inadequate formation of cloud condensation nuclei causing less rain to fall and a significant change in the planet’s albedo.
b) if higher: advanced life forms will experience respiratory impairment or respiratory failure.
388) quantity of fallen leaf litter
a) if lower: inadequate amounts of silica are returned to the soil.
b) if higher: inadequate oxygenation of the soil; damage from fires consuming leaf litter can become too destructive; growth inhibitors in the soil would accumulate.
389) quantity and extent of wetland ecosystems
a) if lower: inadequate burial of organic carbon resulting in too much carbon dioxide in the atmosphere; inadequate habitat and feeding space for a wide variety of bird species.
b) if higher: too much burial of organic carbon resulting in too little carbon dioxide in the atmosphere.
390) quantity of endophytic methanotrophic bacteria in freshwater wetland ecosystems
a) if lower: too much methane will be released to the atmosphere resulting in global warming; inadequate supply of carbon to wetland plants; inadequate denitrification of nitrate.
b) if higher: not enough methane will be released to the atmosphere resulting in global cooling.
391) quantity of marine methanotrophic archaea
a) if lower: too much methane will be released to the atmosphere resulting in global warming; inadequate supply of carbon to wetland plants.
b) if higher: not enough methane will be released to the atmosphere resulting in global cooling.
392) quantity and diversity of viruses in the oceans
a) if lower: inadequate control of planktonic species; inadequate control of algal blooms; impairment of nutrient cycling.
b) if higher: mortality rate for ocean life becomes too high; impairment of nutrient cycling.
393) quantity of termites
a) if lower: inadequate release of methane into the atmosphere resulting in global cooling; inadequate recycling of timber and other celluloid products.
b) if higher: too great a release of methane into the atmosphere resulting in global warming; too much destruction of wooden structures.
394) quantity and diversity of siderophore-secreting bacteria in the oceans
a) if lower: inadequate acquisition of iron by marine life.
b) if higher: too great iron acquisition can lead to the development of deadly algal blooms.
395) quantity of carbon dioxide extracted from the mantle by melting beneath mid-ocean ridges
a) if lower: inadequate rate of release of carbon dioxide into the atmosphere.
b) if higher: too great a rate of release of carbon dioxide into the atmosphere.
396) quantity of carbon dioxide extracted from the mantle by volcanic eruptions
a) if lower: inadequate rate of release of carbon dioxide into the atmosphere.
b) if higher: too great a rate of release of carbon dioxide into the atmosphere.
397) quantity of soil nitrogen
a) if lower: plant growth is limited especially the capacity of plants to remove carbon dioxide from the atmosphere which results in global warming.
b) if higher: nitrogen compounds could reach toxic levels or the growth of plants could be so stimulated that too much carbon dioxide is removed from the atmosphere resulting in global cooling.
398) quantity of marine snow (dead cells, shreds of plankton, bits of faeces, and mineral grains) in the oceans
a) if lower: inadequate release of organic carbon into the deep ocean and ocean bottom for the life forms that reside there; inadequate removal of carbon dioxide from the atmosphere.
b) if higher: too much removal of carbon dioxide from the atmosphere.
399) radiative thermal conductivity of the lower mantle
a) if lower: convection in the mantle will be too vigorous which will make the tectonic plates too unstable and result in too much plate tectonic activity.
b) if higher: convection in the mantle will be too tepid which will result in too weak of a level of plate tectonic activity.
400) average size of aerosol particles in the troposphere
a) if smaller: cloud drop nucleating activity will be too low causing less rain to fall.
b) if larger: cloud nucleating activity will be too high either causing too much rain to fall or causing rainfall to be much less evenly distributed over the planet’s surface.
401) rate of atmospheric dust deposition into the oceans
a) if lower: inadequate infusion of nutrients (iron, phosphorus, nitrogen, etc.) essential for the growth and productivity of plankton.
b) if higher: erosive effects on the continental land masses will disturb and/or destroy many land life forms; productivity and diversity of land life will suffer.
402) level of mixing in the early protoplanetary disk of the solar nebula
a) if lower: proto-Earth would not receive a great enough diversity of elements and compounds.
b) if higher: the development of small bodies in the disk would be too limited; the proto-Earth would be enriched sufficiently in very heavy elements.
References:
1) R. E. Davies and R. H. Koch, “All the Observed Universe Has Contributed to Life,” Philosophical Transactions of the Royal Society of London, Series B, 334 (1991), pp. 391-403.
2) Micheal H. Hart, “Habitable Zones About Main Sequence Stars,” Icarus, 37 (1979), pp. 351-357.
3) William R. Ward, “Comments on the Long-Term Stability of the Earth’s Oliquity,” Icarus, 50 (1982), pp. 444-448.
4) Carl D. Murray, “Seasoned Travellers,” Nature, 361 (1993), p. 586-587.
5) Jacques Laskar and P. Robutel, “The Chaotic Obliquity of the Planets,” Nature, 361 (1993), pp. 608-612.
6) Jacques Laskar, F. Joutel, and P. Robutel, “Stabilization of the Earth’s Obliquity by the Moon,” Nature, 361 (1993), pp. 615-617.
7) H. E. Newsom and S. R. Taylor, “Geochemical Implications of the Formation of the Moon by a Single Giant Impact,” Na- ture, 338 (1989), pp. 29-34.
8) W. M. Kaula, “Venus: A Contrast in Evolution to Earth,” Science, 247 (1990), PP. 1191-1196.
9) Robert T. Rood and James S. Trefil, Are We Alone? The Possibility of Extraterrestrial Civilizations, (New York: Scrib- ner’s Sons, 1983).
10) John D. Barrow and Frank J. Tipler, The Anthropic Cosmological Principle (New York: Oxford University Press, 1986), pp. 510-575.
11) Don L. Anderson, “The Earth as a Planet: Paradigms and Paradoxes,” Science, 22 3 (1984), pp. 347-355.
12) I. H. Campbell and S. R. Taylor, “No Water, No Granite—No Oceans, No Continents,” Geophysical Research Letters, 10 (1983), pp. 1061-1064.
13) Brandon Carter, “The Anthropic Principle and Its Implications for Biological Evolution,” Philosophical Transactions of the Royal Society of London, Series A, 310 (1983), pp. 352-363.
14) Allen H. Hammond, “The Uniqueness of the Earth’s Climate,” Science, 187 (1975), p. 245.
15) Owen B. Toon and Steve Olson, “The Warm Earth,” Science 85, October.(1985), pp. 50- 57.
16) George Gale, “The Anthropic Principle,” Scientific American, 245, No. 6 (1981), pp. 154-171.
17) Hugh Ross, Genesis One: A Scientific Perspective. (Pasadena, California: Reasons to Believe, 1983), pp. 6-7.
18) Ron Cottrell, The Remarkable Spaceship Earth. (Denver, Colorado: Accent Books, 1982).
19) D. Ter Harr, “On the Origin of the Solar System,” Annual Review of Astronomy and Astrophysics, 5 (1967), pp. 267-278.
20) George Greenstein, The Symbiotic Universe. (New York: William Morrow, 1988), pp. 68-97.
21) John M. Templeton, “God Reveals Himself in the Astronomical and in the Infinitesimal,” Journal of the American Scien- tific Affiliation, December 1984 (1984), pp. 196-198.
22) Michael H. Hart, “The Evolution of the Atmosphere of the Earth,” Icarus, 33 (1978), pp. 23-39.
23) Tobias Owen, Robert D. Cess, and V. Ramanathan, “Enhanced CO2 Greenhouse to Compensate for Reduced Solar Lumi- nosity on Early Earth,” Nature, 277 (1979), pp. 640-641.
24) John Gribbin, “The Origin of Life: Earth’s Lucky Break,” Science Digest, May 1983 (1983), pp. 36-102.
25) P. J. E. Peebles and Joseph Silk, “A Cosmic Book of Phenomena,” Nature, 346 (1990), pp. 233-239.
26) Michael H. Hart, “Atmospheric Evolution, the Drake Equation, and DNA: Sparse Life in an Infinite Universe,” in Philoso- phical Cosmology and Philosophy, edited by John Leslie, (New York: Macmillan, 1990), pp. 256-266.
27) Stanley L. Jaki, God and the Cosmologists, (Washington, DC: Regnery Gateway, 1989), pp. 177-184.
28) R. Monastersky, p. “Speedy Spin Kept Early Earth From Freezing,” Science News, 143 (1993), p. 373.
29) The editors, “Our Friend Jove,” Discover. (July 1993) p. 15.
30) Jacques Laskar, “Large-Scale Chaos in the Solar System,” Astronomy and Astrophysics, 287 (1994), pp. 109-113.
31) Richard A. Kerr, “The Solar System’s New Diversity,” Science, 265 (1994), pp. 1360-1362.
32) Richard A. Kerr, “When Comparative Planetology Hit Its Target,” Science 265 (1994), p. 1361.
33) W. R. Kuhn, J. C. G. Walker, and H. G. Marshall, “The Effect on Earth’s Surface Temperature from Variations in Rotation Rate, Continent Formation, Solar Luminosity, and Carbon Dioxide,” Journal of Geophysical Research, 94 (1989), pp. 11,129-131,136.
34) Gregory S. Jenkins, Hal G. Marshall, and W. R. Kuhn, “Pre-Cambrian Climate: The Effects of Land Area and Earth’s Ro- tation Rate,” Journal of Geophysical Research, Series D, 98 (1993), pp. 8785-8791.
35) K. J. Zahnle and J. C. G. Walker, “A Constant Daylength During the Precambrian Era?” Precambrian Research, 37 (1987), pp. 95-105.
36) M. J. Newman and R. T. Rood, “Implications of the Solar Evolution for the Earth’s Early Atmosphere,” Science, 198 (1977), pages 1035-1037.
37) J. C. G. Walker and K. J. Zahnle, “Lunar Nodal Tides and Distance to the Moon During the Precambrian,” Nature, 320 (1986), pp. 600-602.
38) J. F. Kasting and J. B. Pollack, “Effects of High CO2 Levels on Surface Temperatures and Atmospheric Oxidation State of the Early Earth,” Journal of Atmospheric Chemistry, 1 (1984), pp. 403-428.
39) H. G. Marshall, J. C. G. Walker, and W. R. Kuhn, “Long Term Climate Change and the Geochemical Cycle of Carbon,” Journal of Geophysical Research, 93 (1988), pp. 791-801.
40) Pieter G. van Dokkum, et al, “A High Merger Fraction in the Rich Cluster MS 1054-03 at z = 0.83: Direct Evidence for Hierarchical Formation of Massive Galaxies,” Astrophysical Journal Letters, 520 (1999), pp. L95-L98.
41) Anatoly Klypin, Andrey V. Kravtsov, and Octavio Valenzuela, “Where Are the Missing Galactic Satellites?” Astrophysical Journal, 522 (1999), pp. 82-92.
42) Roland Buser, “The Formation and Early Evolution of the Milky Way Galaxy,” Science, 287 (2000), pp. 69-74.
43) Robert Irion, “A Crushing End for our Galaxy,” Science, 287 (2000), pp. 62-64.
44) D. M. Murphy, et al, “Influence of Sea Salt on Aerosol Radiative Properties in the Southern Ocean Marine Boundary Layer, Nature, 392 (1998), pp. 62-65.
45) Neil F. Comins, What If The Moon Didn’t Exist? (New York: HarperCollins, 1993), pp.2-8, 53-65.
46) Hugh Ross, “Lunar Origin Update,” Facts & Faith, v. 9, n. 1 (1995), pp. 1-3.
47) Jack J. Lissauer, “It’s Not Easy to Make the Moon,” Nature 389 (1997), pp. 327-328.
48) Sigeru Ida, Robin M. Canup, and Glen R. Stewart, “Lunar Accretion from an Impact-Generated Disk,” Nature 389 (1997), pp. 353-357.
49) Louis A. Codispoti, “The Limits to Growth,” Nature 387 (1997), pp. 237.
50) Kenneth H. Coale, “A Massive PhytoPlankton Bloom Induced by an Ecosystem-Scale Iron Fertilization Experiment in the Equatorial Pacific Ocean,” Nature 383 (1996), pp. 495-499.
51) P. Jonathan Patchett, “Scum of the Earth After All,” Nature 382 (1996), p. 758.
52) William R. Ward, “Comments on the Long-Term Stability of the Earth’s Oliquity,” Icarus 50 (1982), pp. 444-448.
53) Carl D. Murray, “Seasoned Travellers,” Nature, 361 (1993), pp. 586-587.
54) Jacques Laskar and P. Robutel, “The Chaotic Obliquity of the Planets,” Nature, 361 (1993), pp. 608-612.
55) Jacques Laskar, F. Joutel, and P. Robutel, “Stabilization of the Earth’s Obliquity by the Moon,” Nature, 361 (1993), pp. 615-617.
56) S. H. Rhie, et al, “On Planetary Companions to the MACHO 98-BLG-35 Microlens Star,” Astrophysical Journal, 533 (2000), pp. 378-391.
57) Ron Cowen, “Less Massive Than Saturn?” Science News, 157 (2000), pp. 220-222.
58) Hugh Ross, “Planet Quest—A Recent Success,” Connections, vol. 2, no. 2 (2000), pp. 1-2.
59) G. Gonzalez, “Spectroscopic Analyses of the Parent Stars of Extrasolar Planetary Systems,” Astronomy & Astrophysics 334 (1998): pp. 221-238.
60) Guillermo Gonzalez, “New Planets Hurt Chances for ETI,” Facts & Faith, vol. 12, no. 4 (1998), pp. 2-4.
61) The editors, “The Vacant Interstellar Spaces,” Discover, April 1996, pp. 18, 21.
62) Theodore P. Snow and Adolf N. Witt, “The Interstellar Carbon Budget and the Role of Carbon in Dust and Large Mole- cules,” Science 270 (1995), pp. 1455-1457.
63) Richard A. Kerr, “Revised Galileo Data Leave Jupiter Mysteriously Dry,” Science, 272 (1996), pp. 814-815.
64) Adam Burrows and Jonathan Lumine, “Astronomical Questions of Origin and Survival,” Nature 378 (1995), p. 333.
65) George Wetherill, “How Special Is Jupiter?” Nature 373 (1995), p. 470.
66) B. Zuckerman, T. Forveille, and J,. H. Kastner, “Inhibition of Giant-Planet Formation by Rapid Gas Depletion Around Young Stars,” Nature 373 (1995), pp. 494-496.
67) Hugh Ross, “ Our Solar System, the Heavyweight Champion,” Facts & Faith, v. 10, n. 2 (1996), p. 6.
68) Guillermo Gonzalez, “Solar System Bounces in the Right Range for Life,” Facts & Faith, v. 11, n. 1 (1997), pp. 4-5.
69) C. R. Brackenridge, “Terrestrial Paleoenvironmental Effects of a Late Quaternary-Age Supernova,” Icarus, vol. 46 (1981), pp. 81-93.
70) M. A. Ruderman, “Possible Consequences of Nearby Supernova Explosions for Atmospheric Ozone and Terrestrial Life,” Science, vol. 184 (1974), pp. 1079-1081.
71) G. C. Reid et al, “Effects of Intense Stratospheric Ionization Events,” Nature, vol. 275 (1978), pp. 489-492.
72) B. Edvardsson et al, “The Chemical Evolution of the Galactic Disk. I. Analysis and Results,” Astronomy & Astrophysics, vol. 275 (1993), pp. 101-152.
73) J. J. Maltese et al, “Periodic Modulation of the Oort Cloud Comet Flux by the Adiabatically Changed Galactic Tide,” Ica- rus, vol. 116 (1995), pp 255-268.
74) Paul R. Renne, et al, “Synchrony and Causal Relations Between Permian-Triassic Boundary Crisis and Siberian Flood Volcanism,” Science, 269 (1995), pp. 1413-1416.
75) Hugh Ross, “Sparks in the Deep Freeze,” Facts & Faith, v. 11, n. 1 (1997), pp. 5-6.
76) T. R. Gabella and T. Oka, “Detectiion of H3+ in Interstellar Space,” Nature, 384 (1996), pp. 334-335.
77) Hugh Ross, “Let There Be Air,” Facts & Faith, v. 10, n. 3 (1996), pp. 2-3.
78) Davud J. Des Marais, Harold Strauss, Roger E. Summons, and J. M. Hayes, “Carbon Isotope Evidence for the Stepwise Oxidation of the Proterozoic Environment Nature, 359 (1992), pp. 605-609.
79) Donald E. Canfield and Andreas Teske, “Late Proterozoic Rise in Atmospheric Oxygen Concentration Inferred from Phylogenetic and Sulphur-Isotope Studies,” Nature 382 (1996), pp. 127-132.
80) Alan Cromer, UnCommon Sense: The Heretical Nature of Science (New York: Oxford University Press, 1993), pp. 175- 176.
81) Hugh Ross, “Drifting Giants Highlights Jupiter’s Uniqueness,” Facts & Faith, v. 10, n. 4 (1996), p. 4.
82) Hugh Ross, “New Planets Raise Unwarranted Speculation About Life,” Facts & Faith, volume 10, number 1 (1996), pp. 1- 3.
83) Hugh Ross, “Jupiter’s Stability,” Facts & Faith, volume 8, number 3 (1994), pp. 1-2.
84) Christopher Chyba, “Life BeyondMars,” Nature, 382 (1996), p. 577.
85) E. Skindrad, “Where Is Everybody?” Science News, 150 (1996), p. 153.
86) Stephen H. Schneider, Laboratory Earth: The Planetary Gamble We Can’t Afford to Lose (New York: Basic Books, 1997), pp. 25, 29-30.
87) Guillermo Gonzalez, “Mini-Comets Write New Chapter in Earth-Science,” Facts & Faith, v. 11, n. 3 (197), pp. 6-7.
88) Miguel A. Goñi, Kathleen C. Ruttenberg, and Timothy I. Eglinton, “Sources and Contribution of Terrigenous Organic Car- bon to Surface Sediments in the Gulf of Mexico,” Nature, 389 (1997), pp. 275-278.
89) Paul G. Falkowski, “Evolution of the Nitrogen Cycle and Its Influence on the Biological Sequestration of CO2 in the Ocean,” Nature, 387 (1997), pp. 272-274.
90) John S. Lewis, Physics and Chemistry of the Solar System (San Diego, CA: Academic Press, 1995), pp. 485-492.
91) Hugh Ross, “Earth Design Update: Ozone Times Three,” Facts & Faith, v. 11, n. 4 (1997), pp. 4-5.
92) W. L. Chameides, P. S. Kasibhatla, J. Yienger, and H. Levy II, “Growth of Continental-Scale Metro-Agro-Plexes, Re- gional Ozone Pollution, and World Food Production,” Science, 264 (1994), pp. 74-77.
93) Paul Crutzen and Mark Lawrence, “Ozone Clouds Over the Atlantic,” Nature, 388 (1997), p. 625.
94) Paul Crutzen, “Mesospheric Mysteries,” Science, 277 (1997), pp. 1951-1952.
95) M. E. Summers, et al, “Implications of Satellite OH Observations for Middle Atmospheric H2O and Ozone,” Science, 277 (1997), pp. 1967-1970.
96) K. Suhre, et al, “Ozone-Rich Transients in the Upper Equatorial Atlantic Troposphere,” Nature, 388 (1997), pp. 661-663.
97) L. A. Frank, J. B. Sigwarth, and J. D. Craven, “On the Influx of Small Comets into the Earth’s Upper Atmosphere. II. In- terpretation,” Geophysical Research Letters, 13 (1986), pp. 307-310.
98) David Deming, “Extraterrestrial Accretion and Earth’s Climate,” Geology, in press.
99) T. A. Muller and G. J. MacDonald, “Simultaneous Presence of Orbital Inclination and Eccentricity in Prozy Climate Re- cords from Ocean Drilling Program Site 806,” Geology, 25 (1997), pp. 3-6.
100) Clare E. Reimers, “Feedback from the Sea Floor,” Nature, 391 (1998), pp. 536-537.
101) Hilairy E. Hartnett, Richard G. Keil, John I. Hedges, and Allan H. Devol, “Influence of Oxygen Exposure Time on Organic Carbon Preservation in Continental Margin Sediments,” Nature, 391 (1998), pp. 572-574.
102) Tina Hesman, “Greenhouse Gassed: Carbon Dioxide Spells Indigestion for Food Chains,” Science News, 157 (2000), pp. 200-202.
103) Claire E. Reimers, “Feedbacks from the Sea Floor,” Nature, 391 (1998), pp. 536-537.
104) S. Sahijpal, et al, “A Stellar Origin for the Short-Lived Nuclides in the Early Solar System,” Nature, 391 (1998), pp. 559- 561.
105) Stuart Ross Taylor, Destiny or Chance: Our Solar System and Its Place in the Cosmos (New York: Cambridge University Press, 1998).
106) Peter D. Ward and Donald Brownlee, Rare Earth: Why Complex Life is Uncommon in the Universe (New York: Springer- Verlag, 2000).
107) Dean L. Overman, A Case Against Accident and Self-Organization (New York: Rowman & Littlefield, 1997), pp. 31-150.
108) Michael J. Denton, Nature’s Destiny (New York: The Free Press, 1998), pp. 1-208.
109) D. N. C. Lin, P. Bodenheimer, and D. C. Richardson, “Orbital Migration of the Planetary Companion of 51 Pegasi to Its Present Location,” Nature, 380 (1996), pp. 606-607.
110) Stuart J. Weidenschilling and Francesco Mazari, “Gravitational Scattering as a Possible Origin or Giant Planets at Small Stellar Distances,” Nature, 384 (1996), pp. 619-621.
111) Frederic A. Rasio and Eric B. Ford, “Dynamical Instabilities and the Formation of Extrasolar Planetary Systems,” Science, 274 (1996), pp. 954-956.
112) N. Murray, B. Hansen, M. Holman, and S. Tremaine, “Migrating Planets,” Science, 279 (1998), pp. 69-72.
113) Alister W. Graham, “An Investigation into the Prominence of Spiral Galaxy Bulges,” Astronomical Journal, 121 (2001), pp. 820-840.
114) Fred C. Adams, “Constraints on the Birth Aggregate of the Solar System, Icarus (2001), in press.
115) G. Bertelli and E. Nasi, “Star Formation History in the Solar Vicinity,” Astronomical Journal, 121 (2001), pp. 1013-1023.
116) Nigel D. Marsh and Henrik Svensmark, “Low Cloud Properties Influenced by Cosmic Rays,” Physical Review Letters, 85 (2000), pp. 5004-5007.
117) Gerhard Wagner, et al, “Some Results Relevant to the Discussion of a Possible Link Between Cosmic Rays and the Earth’s Climate,” Journal of Geophysical Research, 106 (2001), pp. 3381-3387.
118) E. Pallé and C. J. Butler, “The Influence of Cosmic Rays on Terrestrial Clouds and Global Warming.” Astronomy & Geo- physics, 41 (2000), pp. 4.19-4.22.
119) B. Gladman and M. J. Duncan, “Fates of Minor Bodies in the Outer Solar System,” Astronomical Journal, 100 (1990), pp. 1680-1693.
120) S. Alan Stern and Paul R. Weissman, “Rapid Collisional Evolution of Comets During the Formation of the Oort Cloud,” Nature, 409 (2001), pp. 589-591.
121) Christopher P. McKay and Margarita M. Marinova, “The Physics, Biology, and Environmental Ethics of Making Mars Habitable,” Astrobiology, 1 (2001), pp. 89-109.
122) Michael Loewenstein, “The Contribution of Population III to the Enrichment and Preheating of the Intracluster Medium,” Astrophysical Journal, 557 (2001), pp. 573-577.
123) Takayoshi Nakamura, et al, “Explosive Nucleosynthesis in Hypernovae,” Astrophysical Journal, 555 (2001), pp. 880-899.
124) Kazuyuki Omukai and Francesco Palla, “On the Formation of Massive Primordial Stars,” Astrophysical Journal Letters, 561 (2001), pp. L55-L58.
125) Renu Malhotra, Matthew Holman, and Takashi Ito, “Chaos and Stability of the Solar System,” Proceedings of the National Academy of Sciences, 98 (2001), pp. 12342-12343.
126) Takashi Ito and Kujotaka Tanikawa, “Stability and Instability of the Terrestrial Protoplanet System and Their Possible Roles in the Final Stage of Planet Formation,” Icarus, 139 (1999), pp. 336-349.
127) Li-Chin Yeh and Ing-Guey Jiang, “Orbital Evolution of Scattered Planets,” Astrophysical Journal, 561 (2001), pp. 364- 371.
128) M. Massarotti, A. Iovino, and A. Buzzoni, “Dust Absorption and the Cosmic Ultraviolet Flux Density,” Astrophysical Journal Letters, 559 (2001), pp. L105-L108.
129) Kentaro Nagamine, Masataka Fukugita, Renyue Cen, and Jeremiah P. Ostriker, “Star Formation History and Stellar Metal- licity Distribution in a Cold Dark Matter Universe,” Astrophysical Journal, 558 (2001), pp. 497-504.
130) Revyue Cen, “Why Are There Dwarf Spheroidal Galaxies?” Astrophysical Journal Letters, 549 (2001), pp. L195-L198.
131) Martin Elvis, Massimo Marengo, and Margarita Karovska, “Smoking Quasars: A New Source for Cosmic Dust,” Astro- physical Journal Letters, 567 (2002), pp. L107-L110.
132) N, Massarotti. A. Iovino, and A. Buzzoni, “Dust Absorption and the Cosmic Ultraviolet Flux Density,” Astrophysical Journal Letters, 559 (2001), pp. L105-L108.
133) James Wookey, J. Michael Kendall, and Guilhem Barruol, “Mid-Mantle Deformation Inferred from Seismic Anistropy,” Nature, 415 (2002), pp. 777-780.
134) Karen M. Fischer, “flow and Fabric Deep Down,” Nature, 415 (2002), pp. 745-748.
135) Klaus Regenauer-Lieb, Dave A. Yuen, and Joy Branlund, “The Initiation of Subduction: Criticality by Addition of Water?” Science, 294 (2001), pp. 578-580.
136) Leon Barry, George C. Craig, and John Thuburn, “Poleward Heat Transport by the Atmospheric Heat Engine,” Nature, 415 (2002), pp. 774-777.
137) Akira Kouchi, et al, “Rapid Growth of Asteroids Owing to Very Sticky Interstellar Organic Grains,” Astrophysical Journal Letters, 566 (2002), pp. L121-L124.
138) Christian J. Bjerrum and Donald E. Canfield, “Ocean Productivity Before About 1.9 Gyr Ago Limited by Phosphorus Ad- sorption onto Iron Oxides,” Nature, 417 (2002), pp. 159-162.
139) David E. Harker and Steven J. Desch, “Annealing of Silicate Dust by Nebular Shocks at 10 AU,” Astrophysical Journal Letters, 565 (2002), pp. L109-L112.
140) Chadwick A. Trujillo, David C. Jewitt, and Jane X. Luu, “Properties of the Trans-Neptunian Belt: Statistics from the Can- ada-France-Hawaii Telescope Survey,” Astronomical Journal, 122 (2001), pp. 457-473.
141) W. A. Dziembowski, P. R. Goode, and J. Schou, “Does the Sun Shrink with Increasing Magnetic Activity?” Astrophysical Journal, 553 (2001), pp. 897-904.
142) Anthony Aguirre, et al, “Metal Enrichment of the Intergalactic Medium in Cosmological Simulations,” Astrophysical Journal, 561 (2001), pp. 521-549.
143) Ron Cowen, “Cosmic Remodeling: Superwinds Star in Early Universe,” Science News, 161 (2002), p. 244.
144) Tom Abel, Greg L. Byran, and Michael L. Norman, “The Formation of the First Star in the Universe,” Science, 295 (2002), pp. 93-98.
145) Robert Irion, “The Quest for Population III,” Science, 295 (2002), pp. 66-67.
146) Y.-Z. Qian, W. L. W. Sargent, and G. J. Wasserburg, “The Prompt Inventory from Very Massive Stars and Elemental Abundances in Lya Systems,” Astrophysical Journal Letters, 569 (2002), pp. L61-L64.
147) Kazuyuki Omukai and Francesco Palla, “On the Formation of Massive Primordial Stars,” Astrophysical Journal Letters, 561 (2001), pp. L55-L58.
148) A. Heger and S. E. Woosley, “The Nucleosynthetic Signature of Population III,” Astrophysical Journal, 567 (2002), pp. 532-543.
149) Michael Loewenstein, “The Contribution of Population III to the Enrichment and Preheating of the Intracluster Medium,” Astrophysical Journal, 557 (2001), pp. 573-577.
150) Takayoshi Makamura, et al, “Explosive Nucleosynthesis in Hypernovae,” Astrophysical Journal, 555 (2001), pp. 880-899.
151) Steve Dawson, et al, “A Galactic Wind at z = 5.190,” Astrophysical Journal, 570 (2002), pp. 92-99.
152) John E. Norris, et al, “Extremely Metal-Poor Stars. IX. CS 22949-037 and the Role of Hypernovae,” Astrophysical Journal Letters, 569 (2002), pp. L107-110.
153) Daniel R. Bond, “Electrode-Reducing Microorganisms That Harvest Energy from Marine Sediments,” Science, 295 (2002), pp. 483-485.
154) E. L. Martin, et al, “Four Brown Dwarfs in the Taurus Star-Forming Region,” Astrophysical Journal Letters, 561 (2001), pp. L195-L198.
155) Tom Fenchel, “Marine Bugs and Carbon Flow,” Science, 292 (2001), pp. 2444-2445.
156) Zbigniew S. Kolber, et al, “Contribution of Aerobic Photoheterotrophic Bacteria to the Carbon Cycle in the Ocean,” Sci- ence, 292 (2001), pp. 2492-2495.
157) Martin J. Rees. “How the Cosmic Dark Age Ended,” Science, 295 (2002), pp. 51-53.
158) Jay Melosh, “A New Model Moon,” Nature, 412 (2001), pp. 694-695.
159) Robin M. Canup and Erik Asphaug, “Origin of the Moon in a Giant Impact Near the End of the Earth’s Formation,” Na- ture, 412 (2001), pp. 708-712.
160) M. Elvis G. Risaliti, and G. Zamorani, “Most Supermassive Black Holes Must Be Rapidly Rotating,” Astrophysical Jour- nal Letters, 565 (2002), pp. L75-L77.
161) M. Pätzold and H. Rauer, “Where Are the Massive Close-In Extrasolar Planets?” Astrophysical Journal Letters, 568 (2002), pp. L117-L120.
162) Shay Zucker and Tsevi Mazeh, “On the Mass-Period Correlation of the Extrasolar Planets,” Astrophysical Journal Letters, 568 (2002), pp. L113-L116.
163) B. S. Gaudi, et al, “Microlensing Constraints on the Frequency of Jupiter-Mass Companions: Analysis of 5 Years of Planet Photometry,” Astrophysical Journal, 566 (2002), pp. 463-499.
164) Motohiko Murakami, et al, “Water in Earth’s Lower Mantle,” Science, 295 (2002), pp. 1885-1887.
165) Lee Hartmann, Javier Ballesteros-Paredes, and Edwin A. Bergin, “Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood,” Astrophysical Journal, 562 (2001), pp. 852-868.
166) Renyue Cen, “Why Are There Dwarf Spheroidal Galaxies?” Astrophysical Journal Letters, 549 (2001), pp. L195-L198.
167) Thilo Kranz, Adrianne Slyz, and Hans-Walter Rix, “Probing for Dark Matter Within Spiral Galaxy Disks,” Astrophysical Journal, 562 (2001), pp. 164-178.
168) Francesco Gertola, “Putting Galaxies on the Scale,” Science, 295 (2002), pp. 283-284.
169) David R. Soderblom, Burton F. jones, and Debra Fischer, “Rotational Studies of Late-Type Stars. VII. M34 (NGC 1039) and the Evolution of Angular Momentum and Activity in Young Solar-Type Stars,” Astrophysical Journal, 563 (2001), pp. 334-340.
170) John Scalo and J. Craig Wheeler, “Astrophysical and Astrobiological Implications of Gamma-Ray Burst Properties,” As- trophysical Journal, 566 (2002), pp. 723-737.
171) Jan van Paradijs, “From Gamma-Ray Bursts to Supernovae,” Science, 286 (1999), pp. 693-695.
172) J. S. Bloom, S. R. Kulkarni, and S. G. Djorgovski, “The Observed Offset Distribution of Gamma-Ray Bursts from Their Host Galaxies: A Robust Clue to the Nature of the Progenitors,” Astronomical Journal, 123 (2002), pp. 1111-1148.
173) Colin D. O’Dowd, et al, “Atmospheric Particles From Organic Vapours,” Nature, 416 (2002), p. 497.
174) E. W. Cliver and A. G. Ling, “22 Year Patterns in the Relationship of Sunspot Number and Tilt Angle to Cosmic-Ray In- tensity,” Astrophysical Journal Letters, 551 (2001), pp. L189-L192.
175) Kentaro Nagamine, Jeremiah P. Ostriker, and Renyue Cen, “Cosmic Mach Number as a Function of Overdensity and Gal- axy Age,” Astrophysical Journal, 553 (2001), pp. 513-527.
176) John E. Gizis, I. Neill Reid, and Suzanne L. Hawley, “The Palomar/MSU Nearby Star Spectroscopic Survey. III. Chro- mospheric Activity, M Dwarf Ages, and the Local Star Formation History,” Astronomical Journal, 123 (2002), pp. 3356-3369
177) Jason Pruet, Rebecca Surman, and Gail C. McLaughlin, “On the Contribution of Gamma-Ray Bursts to the Galactic Inven- tory of Some Intermediate-Mass Nuclei,” Astrophysical Journal Letters, 602 (2004), pp. L101-L104.
178) V. A. Dogiel , E. Schönfelder, and A. W. Strong, “The Cosmic Ray Luminosity of the Galaxy,” Astrophysical Journal Let- ters, 572 (2002), pp. L157-L159.
179) Ken Croswell, The Alchemy of the Heavens (New York: Anchor Books, 1995).
180) John Emsley, The Elements, third edition (Oxford, UK: Clarendon Press, 1998), pp. 24, 40, 56, 58, 60, 62, 78, 102, 106, 122, 130, 138, 152, 160, 188, 198, 214, 222, 230.
181) Ron Cowen, “Celestial Divide,” Science News. 162 (2002), pp. 244-245.
182) Ron Cowen, “Cosmic Remodeling : Superwinds Star in Early Universe,” Science News, 161 (2002), p. 244.
183) Jason Tumlinson, Mark L. Giroux, and J. Michael Shull, “Probing the first stars with hydrogen and helium recombination emission,” Astrophysical Journal Letters, 550 (2002), pp. L1-L5.
184) Y.-Z. Qian, W.L.W. Sargent, and G.J. Wasserburg, “The prompt inventory from very massive stars and elemental abun- dances in Lya systems,” Astrophysical Journal Letters, 569 (2002), pp. L61-L64.
185) Steve Dawson, Hyron Spinrad, et al., “A Galactic Wind AT z = 5.190,” Astrophysical Journal 570 (2002), pp. 92-99.
186) John E. Norris, Sean G. Ryan, Timothy C. Beers and Wako Aoki and Hiroyasu Ando, “Extremely metal-poor stars. IX. CS 22949-037 and the role of hypernovae,” Astrophysical Journal Letters, 569 (2002), pp. L107-L110.
187) Martin Elvis, Massimo Marengo and Margarita Karovska, “Smoking Quasars: A New Source for Cosmic Dust,” Astro- physical Journal Letters, 567 (2002), pp. L107-L110.
188) Mark G. Lawrence, “Side Effects of Oceanic Iron Fertilization,” Science, 297 (2002), p. 1993.
189) Charles E. Kolb, “Iodine’s Air of Importance,” Nature, 417 (2002), pp. 597-598.
190) Colin D. O’Dowd, et al, “Marine Aerosol Formation from Biogenic Iodine Emissions,” Nature, 417 (2002), pp. 632-636.
191) Richard A. Kerr, “Mantle Plumes Both Tall and Short?” Science, 302 (2003), p. 1643.
192) Todd A. Thompson, “Magnetic Protoneutron Star Winds and r-Process Nucleosynthesis,” Astrophysical Journal Letters, 585 (2003), pp. L33-L36.
193) Andrei M. Beloborodov, “Nuclear Composition of Gamma-Ray Burst Fireballs,” Astrophysical Journal, 588 (2003), pp. 9331-944.
194) Jason Pruet, Rebecca Surman, and Gail C. McLaughlin, “On the Contribution of Gamma-Ray Bursts to the Galactic Inven- tory of Some Intermediate-Mass Nuclei,” Astrophysical Journal Letters, 602 (2004), pp. L101-L104.
195) Sydney A. Barnes, “A Connection Between the Morphology of the X-Ray Emission and Rotation for Solar-Type Stars in Open Clusters,” Astrophysical Journal Letters, 586 (2003), pp. L145-L147.
196) Jonathan Arons, “Magnetars in the Metagalaxy: An Origin of Ultra-High Energy Cosmic Rays in the Nearby Universe,” Astrophysical Journal, 589 (2003), pp. 871-892.
197) Shri Kulkarni, “The Missing Link,” Nature, 419 (2002), pp. 121-123.
198) F. P. Gavriil, V. M. Kaspi, and P. W. Woods, “Magnetar-Like X-Ray Bursts from an Anomalous X-Ray Pulsar,” Nature, 419 (2002), pp. 142-144.
199) Harold F. Levinson and Alessandro Morbidelli, “The Formation of the Kuiper Belt by the Outward Transport of Bodies During Neptune’s Migration,” Nature, 426 (2003), pp. 419-421.
200) Rosemary A. Mardling and D. N. C. Lin, “Calculating the Tidal, Spin, and Dynamical Evolution of Extrasolar Planetary Systems,” Astrophysical Journal, 573 (2002), pp. 829-844.
201) Yu N. Mishurov and L. A. Zenina, “Yes, the Sun is Located Near the Corotation Circle,” Astronomy & Astrophysics, 341 (1999), pp. 81-85.
202) Guillermo Gonzalez, “Is the Sun Anomalous?” Astronomy & Geophysics, 40 (1999), pp. 25-30.
203) J. L. Turner, et al, “An Extragalactic Supernebula Confined by Gravity,” Nature, 423 (2003), pp. 621-623.
204) Wolf U. Reimold, “Impact Cratering Comes of Age,” Science, 300 (2003), pp. 1889-1890.
205) Andrey V. Kravtsov, “On the Origin of the Global Schmidt Law of Star Formation,” Astrophysical Journal Letters, 590 (2003), pp. L1-L4.
206) Keiichi Wada and Aparna Venkatesan, “Feedback from the First Supernovae in Protogalaxies: The Fate of the Generated Metals,” Astrophysical Journal, 591 (2003), pp. 38-42.
207) Renyue Cen, “The Implications of Wilkinson Microwave Anisotropy Probe Observations for Population III Star Formation Processes,” Astrophysical Journal Letters, 591 (2003), pp. L5-L8.
208) Renyue Cen, “The Universe Was Reionized Twice,” Astrophysical Journal, 591 (2003), pp. 12-37.
209) Hans Kepler, Michael Wiedenbeck, and Svyatoslav S. Shcheka, “Carbon Solubility in Olivine and the Mode of Carbon Storage in the Earth’s Mantle,” Nature, 424 (2003), pp. 414-416.
210) Mario G. Abadi, et al, “Simulations of Galaxy Formation in a L Cold Dark Matter Universe. I. Dynamical and Photometric Properties of Simulated Disk Galaxy,” Astrophysical Journal, 591 (2003), pp. 499-514.
211) K. Pfeilsticker, et al, “Atmospheric Detection of Water Dimers Via Near-Infrared Absorption,” Science, 300 (2003), pp. 2078-2080.
212) A. Finoguenov, A. Burkert, and H. Böhringer, “Role of Clusters of Galaxies in the Evolution of the Metal Budget in the Universe,” Astrophysical Journal, 594 (2003), pp. 136-143.
213) Marc J. Kuchner. “Volatile-Rich Earth-Mass Planets in the Habitable Zone,” Astrophysical Journal Letters, 596 (2003), pp. L105-L108.
214) KenjiBekki and Warrick J. Couch, “Starbursts from the Strong Compression of Galactic Molecular Clouds Due to the High Pressure of the Intracluster Medium,” Astrophysical Journal Letters, 596 (2003), pp. L13-L16.
215) S. Chakrabarti, G. Laughlin, and F. H. Shu, “Branch, Spur, and Feather Formation in Spiral Galaxies,” Astrophysical Jour- nal, 596 (2003), pp. 220-239.
216) Edward W. Thommes and Jack J. Lissauer, “Resonant Inclination Excitation of Migrating Giant Planets,” Astrophysical Journal, 597 (2003), pp. 566-580.
217) J. B. Adams, M. E. Mann, and C. M. Ammann, “Proxy Evidence for an El Nino-Like Response to Volcanic Forcing,” Na- ture, 426 (2003), pp. 274-278.
218) Shanaka de Silva, “Eruptions Linked to El Nino,” Nature, 426 (2003), pp. 239-241.
219) J. S. Seewald, “Organic-Inorganic Interactions in Petroleum-Producing Sedimentary Basins,” Nature, 426 (2003), pp. 327- 333.
220) I. M. Head, D. M. Jones, and S. R. Larter, “Biological Activity in the Deep Subsurface and the Origin of Heavy Oil,” Na- ture, 426 (2003), pp. 344-352.
221) N. White, M. Thompson, and T. Barwise, “Understanding the Thermal Evolution of Deep-Water Continental Margins, Na- ture, 426 (2003), pp. 334-343.
222) Anthony C. Harris, et al, “Melt Inclusions in Veins: Linking Magmas and Porphyry Cu Deposits,” Science, 302 (2003), pp. 2109-2111.
223) Jean S. Cline, “How to Concentrate Copper,” Science, 302 (2003), pp. 2075-2076.
224) Takaya Nozawa, et al, “Dust in the Early Universe: Dust Formation in the Ejecta of Pupulation III Supernovae,” Astro- physical Journal, 598 (2003), PP. 785-803.
225) David Stevenson, “Inside History in Depth,” Nature, 428 (2004), pp. 476-477.
226) Linda T. Elkins-Tantour, Bradford H. Hager, and Timothy L. Grove, “Magmatic Effects of the Late Heavy Bombardment,” Earth and Planetary Science Letters, 222 (2004), pp. 17-27.
227) Carl B. Agee, “Earth Science: Hot Metal,” Nature 429 (2004): 33-35.
228) David C. Rubie, Christine K. Gessmann, and Daniel J. Frost, “Partitioning of Oxygen During Core formation on the Earth and Mars,” Nature, 429 (2004), pp. 58-61.
229) A. Mobidelli, et al, “A Plausible Cause of the Late Heavy Bombardment,” Meteoritics & Planetary Science, 36 (2001), pp. 371-380.
230) R. Gomes, et al, “Origin of the Cataclysmic Late Heavy Bombardment Period of the Terrestrial Planets,” Nature, 435 (2005), pp. 466-469.
231) J. Lelieveld, P. J. Crutzen, and F. J. Dentener, “Changing Concentration , Lifetimes, and Climate Forcing of Atmospheric Methane,” Tellus B, 50 (1998), pp. 128-150.
232) J. T. Houghton, et al, Climate Change 2001: The Scientific Basis (Cambridge, UK: Cambridge University Press, 2001).
233) J. T, G. Hamilton, et al, “Chloride Methlation by Plant Pectin: An Efficient Environmentally Significant Process,” Science, 301 (2003), pp. 206-209.
234) Frank Keppler, et al, “Methane Emissions from Terrestrial Plants Under Aerobic Conditions,” Nature, 439 (2006), pp. 187- 191.
235) Naoki Yoshida, Volker Bromm, and Lars Hernquist,, “The Era of Massive Population III Stars: Cosmological Implications and Self-Termination,” The Astrophysical Journal, 605, (2004), pp. 579-590.
236) Xin Yang, et al, “Tropospheric Bromine Chemistry and Its Impact on Ozone: A Model Study,” Journal of Geophysical Re- search, 110, issue D33 (2005), citation ID D23311.
237) Ross J. Salawitch, “Biogenic Bromine,” Nature, 439 (2006), pp. 275-276.
238) A. B. Verchovsky, I. P. Wright, and C. T. Pillinger, “Astrophysical Significance of Asymptotic Giant Branch Stellar Wind Energies Recorded in Meteoritic SiC Grains,” Astrophysical Journal, 619 (2004), pp. 611-619.
239) George W. Koch, et al, “The Limits to Tree Height,” Nature, 428 (2004), pp. 851-854.
240) Ian Woodward, “Tall Storeys,” Nature, 428 (2004), pp. 807-808.
241) Amr A. El-Zant, et al, “Flat-Cored Dark Matter in Cuspy Clusters of Galaxies,” Astrophysical Journal Letters, 607 (2004), pp. L75-L78.
242) Douglas Clowe, Anthony Gonzalez, and Maxim Markevitch, “Weak-Lensing Mass Reconstruction of the Interacting Clus- ter IE 0657-558: Direct Evidence for the Existence of Dark Matter,” Astrophysical Journal, 604 (2004), pp. 596-603.
243) Andreas Heithausen,, “Molecular Hydrogen as Baryonic Dark Matter,” The Astrophysical Journal Letters, 606 (2004), pp. L13-L15.
244) Tommaso Treu and Léon V. E. Koopmans, “Massive Dark Matter Halos and Evolution of Early-Type Galaxies to z = 1,” Astrophysical Journal, 611 (2004), pp. 739-760.
245) Paul Martin and Luis C. Ho, “A Population of Massive Globular Clusters in NGC 5128,” Astrophysical Journal, 610 (2004), pp. 233-246.
246) Kenneth V. Beard, Harry T. Ochs III, and Cynthia H. Twohy, “Aircraft Measurements of High Average Charges on Cloud Drops in Layer Clouds,” Geophysical Research Letters, 31 (2004), L14111, doi:10.1029/2004GL020465.
247) S. Cazaux and M. Spaans, “Molecular Hydrogen Formation on Dust Grains in the High-Redshift Universe,” Astrophysical Journal, 611 (2004), pp. 40-51.
248) Rupali Chandar, et al, “The Globular Cluster Systems of Five Nearby Spiral Galaxies: New Insights from Hubble Space Telescope Imaging,” Astrophysical Journal, 611 (2004), pp. 220-244.
249) Susan G. Neff, James S. Ulvestad, and Stacy H. Teng, “A Supernova Factory in the Merger System ARP 299,” Astrophysi- cal Journal, 611 (2004), pp. 186-199.
250) Carolyn M. Aitken, D. M. Jones, and S. R. Larter, “Anaerobic Hydrocarbon Biodegradation in Deep Subsurface Oil Reser- voirs,” Nature, 431 (2004), pp. 291-294.
251) Fred C. Adams, et al, “Photoevaporation of Circumstellar Disks Due to External Far-Ultraviolet Radiation in Stellar Ag- gregates,” Astrophysical Journal, 611 (2004), pp. 360-379.
252) Tommaso Treu and Léon V. E. Koopmans, “Massive Dark Matter Halos and Evolution of Early-Type Galaxies to z = 1,” Astrophysical Journal, 611 (2004), pp. 739-760.
253) Munir Humayun, Liping Qin, and Marc D. Norman, “Geochemical Evidence for Excess Iron in the Mantle Beneath Ha- waii,” Science, 306 (2004), pp. 91-94.
254) Cin-Ty Aeolus Lee, “Are Earth’s Core and Mantle on Speaking Terms?” Science, 306 (2004), pp. 64-65.
255) Alexandra Goho, “Deep Squeeze: Experiments Point to Methane in Earth’s Mantle,” Science News, 166 (2004), p. 198.
256) Alexandra Goho, “Deep Squeeze: Experiments Point to Methane in Earth’s Mantle,” Science News, 166 (2004), p. 198.
257) Kim A. Venn, et al, “Stellar Chemical Signatures and Hierarchical Galaxy Formation,” Astronomical Journal, 128 (2004), pp. 1177-1195.
258) Martin Solan, et al, “Extinction and Ecosystem Function in the Marine Benthos,” Science, 306 (2004), pp. 1177-1180.
259) Steven F. Maria, et al, “Organic Aerosol Growth Mechanisms and Their Climate-Forcing Implications,” Science, 306 (2004), pp. 1921-1924.
260) Alessandro Morbidelli, “How Neptune Pushed the Boundaries of Our Solar System,” Science, 306 (2004), pp. 1302-1304.
261) Harold F. Levison and Alessandro Morbidelli, “The Formation of the Kuiper Belt by the Outward Transport of Bodies During Neptune’s Migration,” Nature, 426 (2003), pp. 419-421.
262) Rodney S. Gomes, Alessandro Morbidelli, and Harold F. Levison, “Planetary Migration in a Planetesimal Disk: Why did Neptune Stop at 30 AU?” Icarus, 170 (2004), pp. 492-507.
263) Rodney S. Gomes, “The Origin of the Kuiper Belt High-Inclination Population,” Icarus, 161 (2003), pp. 404-418.
264) Richard A. Kerr, “Did Jupiter and Saturn Team Up to Pummel the Inner Solar System? Report from the November 8-12, 2004 Meeting of the Division for Planetary Sciences at Louisville, Kentucky,” Science, 306 (2004), p. 1676.
265) Paul W. J. J. van der Wielen, et al, “The Enigma of Prokaryotic Life in Deep Hypersaline Anoxic Basins,” Science, 307 (2005), pp. 121-123.
266) B. R. McNamara, et al, “The Heating of Gas in a Galaxy Cluster by X-Ray Cavities and Large-Scale Shock Fronts,” Na- ture, 433 (2005), pp. 45-47.
267) Dave Waltham, “Anthropic Selection for the Moon’s Mass,” Astrobiology, 4 (2004), pp. 460-468.
268) Samir Salim, et al, “New Constraints on the Star Formation Histories and Dust Attentuation of Galaxies in the Local Uni- verse from GALEX,” Astrophysical Journal Letters, 619 (2005), pp. L39-L42.
269) I. D. Karachentsev, “The Local Group and Other Neighboring Galaxy Groups,” Astronomical Journal, 129 (2005), pp. 178-188.
270) Hans O. U. Fynbo, “Revised Rates for the Stellar Triple-Alpha Process from Measurement of 12C Nuclear Resonances,” Nature, 433 (2005), pp. 136-139.
271) Isabelle A. Grenier, Jean-Marc Casandjian, and Régis Terrier, “Unveiling Extensive Clouds of Dark Gas in the Solar Neighborhood,” Science, 307 (2005), pp. 1292-1295.
272) Sharon Kedar and Frank H. Webb. “The Ocean’s Seismic Hum,” Science, 307 (2005), pp. 682-683.
273) Hidenori Genda and Yutaka Abe, “Enhanced Atmospheric Loss on Protoplanets at the Giant Impact Phase in the Presence of Oceans,” Nature, 433 (2005), pp. 842-844.
274) Kevin Zahnle, “Planetary Science: Being There,” Nature 433 (2005): 814-815.
275) Fabrizio Nicastro, et al, “The Mass of the Missing Baryons in the X-Ray Forest of the Warm-Hot Intergalactic Medium,” Nature, 433 (2005), pp. 495-498.
276) Isabelle Basile-Doelsch, Jean Dominique Meunier, and Claude Parron, “Another Continental Pool in the Terrestrial Silicon Cycle,” Nature, 433 (2005), pp. 399-402.
277) Ruprecht Jaenicke, “Abundance of Cellular Material and Proteins in the Atmosphere,” Science, 308 (2005), p. 73.
278) Louis A. Derry, et al, “Biological Control of Terrestrial Silica Cycling and Export Fluxes to Watersheds,” Nature, 433 (2005), pp. 728-731.
279) Robert Bailis, Majid Ezzati, and Daniel M. Kammen, “Mortality and Greenhouse Gas Impacts of Biomass and Petroleum Energy Futures in Africa,” Science, 308 (2005), pp. 98-103.
280) Volker Springel, Tiziana Di Matteo, and Lars Hernquist, “Black Holes in Galaxy Mergers: The Formation of Red Elliptical Galaxies,” Astrophysical Journal Letters, 620 (2005), pp. L79-L82.
281) Ping He, Long-Long Feng, and Li-Zhi Fang, “Distributions of the Baryon Fraction on Large Scales in the Universe,” As- trophysical Journal, 623 (2005), pp. 601-611.
282) S. Dye and S. J. Warren, “Decomposition of the Visible and Dark Matter in the Einstein Ring 0047-2808 by Semilinear In- version,” Astrophysical Journal, 623 (2005), pp. 31-41.
283) Neville J. Woolf, “What Is an Earth-Like Planet?” Abstract # 926, Abstracts of the Biennial Meeting of the NASA Astro- biology Institute, April 10-14, 2005, Astrobiology, 5 (2005), pp. 186-187.
284) M. L. Ceccarelli, et al, “Galaxy Peculiar Velocities and Infall onto Groups,” Astrophysical Journal, 622 (2005), pp. 853- 861.
285) Jason Tomlinson and Taotao Fang, “Hot Baryons and the Distribution of Metals in the Intergalactic Medium,” Astrophysi- cal Journal Letters, 623 (2005), pp. L97-L100.
286) Edward Belbruno and J. Richard Gott III, “Where Did the Moon Come From?” Astronomical Journal, 129 (2005), pp. 1724-1745.
287) John Bally, Nick Moeckel, and Henry Throop, “Planet Formation in OB Associations,” Abstract # 743, Abstracts of the Biennial Meeting of the NASA Astrobiology Institute, April 10-14, 2005, Astrobiology, 5 (2005), pp. 186-187.
288) Henry B. Throop and John Bally, “Can Photoevaporation Trigger Planetesimal Formation?” Astrophysical Journal Letters, 623 (2005), pp. L149-L152.
289) James Lyons and Edward Young, “The Formation Environment of the Solar Nebula as Inferred from Oxygen Isotopes in Meteorites,” Abstract # 990, Abstracts of the Biennial Meeting of the NASA Astrobiology Institute, April 10-14, 2005, As- trobiology, 5 (2005), pp. 186-187.
290) B. W. Holwerda, et al, “The Opacity of Spiral Galaxy Disks. III. Automating the Synthetic Field Method,” Astronomical Journal, 129 (2005), pp. 1381-1395.
291) B. W. Holwerda, et al, “The Opacity of Spiral Galaxy Disks. IV. Radial Extinction Profiles from Counts of Distant Galax- ies Seen Through Foreground Disks,” Astronomical Journal, 129 (2005), pp. 1396-1411.
292) Zoë M. Leinhardt and Derek C. Richardson, “Planetesimals to Protoplanets: Effect of Fragmentation on Terrestrial Planet Formation,” Astrophysical Journal, 625 (2005), pp. 427-440.
293) Zoë M. Leinhardt and Derek C. Richardson, “Planetesimal Evolution and Terrestrial Planet Formation,” Abstract # 975, Abstracts of the Biennial Meeting of the NASA Astrobiology Institute, April 10-14, 2005, Astrobiology, 5 (2005), p. 182.
294) James L.Green, et al, “On the Origin of Whistler Mode Radiation in the Plasmasphere,” Journal of Geophysical Research, 110, Issue A3, (2005), Cite ID A03201.
295) D. R. Gies and J. W. Helsel, “Ice Age Epochs and the Sun’s Path Through the Galaxy,” Astrophysical Journal, 626 (2005), pp. 844-848.
296) S. Mostefaoui, G. W. Lugmair, and P. Hoppe, “60Fe: A Heat Source for Planetary Differentiation from a Nearby Supernova Explosion,” Astrophysical Journal, 625 (2005), pp. 271-277.
297) Beth Willman, et al, “A New Milky Way Dwarf Galaxy in Ursa Major,” Astrophysical Journal Letters, 626 (2005), pp. L85-L88.
298) Brian W. O’Shea, Tom Abel, Dan Whalen, and Micheal L. Norman, “Forming a Primordial Star in a Relic H II Region,” Astrophysical Journal 628 (2005): L5-L8.
299) Amos Banin, “The Enigma of the Martian Soil,” Science 309 (2005): 888-90.
300) Jason Gans, Murray Wolinsky, and John Dunbar, “Computational Improvements Reveal Great Bacterial Diversity and High Metal Toxicity in Soil,” Science 309 (2005): 1387-90.
301) Ashna A. Raghoebarsing et al., “Methanotrophic Symbionts Provide Carbon for Photosynthesis in Peat Bogs,” Nature 436 (2005): 1153-56.
302) Scott Messenger, Lindsay P. Keller, and Dante S. Lauretta, “Supernova Olivine from Cometary Dust,” Science 309 (2005): 737-41.
303) Robert G. Strom et al., “The Origin of Planetary Impactors in the Inner Solar System,” Science 309 (2005): 1847-50.
304) Robert Irion, “Astronomers Sweep Space for the Sources of Cosmic Dust,” Science 310 (2005): 614-15.
305) Curtis A. Suttle, “Viruses in the Sea,” Nature 437 (2005): 356-61.
306) A. Kashlinsky, “Cosmic Infrared Background from Population III Stars and Its Effect on Spectra of High-z Gamma-Ray Bursts,” Astrophysical Journal 633 (2005): L5-L8.
307) Wilton S. Dias and J. R. D. Lépine, “Direct Determination of the Spiral Pattern Rotation Speed of the Galaxy,” Astrophysi- cal Journal 629 (2005): 825-31.
308) Kevin R. Arrigo, “Marine Microorganisms and Global Nutrient Cycles,” Nature, 437 (2005), pp. 349-355.
309) F. S. Chapin, III et al., “Role of Land-Surface Changes in Arctic Summer Warming,” Science 310 (2005): 657-60.
310) David Martínez-Delgado et al., “The Closest View of a Dwarf Galaxy: New Evidence on the Nature of the Canis Major Overdensity,” Astrophysical Journal 633 (2005): 205-09.
311) Verne V. Smith et al., “Fluorine Abundance Variations in Red Giants of the Globular Cluster M4 and Early-Cluster Chemical Pollution,” Astrophysical Journal 633 (2005): 392-97.
312) Y. Zhang and X.-W. Liu, “Fluorine Abundances in Planetary Nebulae,” Astrophysical Journal 631 (2005): L61-64.
313) Quirin Schiermeier, “Methane Finding Baffles Scientists,” Nature 439 (2006): 128.
314) Ross J. Salawitch, “Atmospheric Chemistry: Biogenic Bromine,” Nature 439 (2006): 275-77.
315) Xin Yang et al., “Tropospheric Bromine Chemistry and Its Impact on Ozone: A Model Study,” Journal of Geophysical Re- search, vol. 10, iss. D23, CiteID D23311.
316) Sigurdur R. Gislason, Eric H. Oelkers, and Arni Snorrason, “Role of River-Suspended Material in the Global Carbon Cy- cle,” Geology 34, no. 1 (2006): 49-52.
317) Roland Diehl et al., “Radioactive 26Al from Massive Stars in the Galaxy,” Nature 439 (2006): 45-47.
318) Hsiao-Wen Chen et al., “Echelle Spectroscopy of a Gamma-ray Burst Afterglow at z= 3.969: A New Probe of the Interstel- lar and Intergalactic Media in the Young Universe,”Astrophysical Journal 634 (2005): L25-28.
319) Giulio Di Toro et al., “Natural and Experimental Evidence of Melt Lubrication of Faults During Earthquakes,” Science 311 (2006): 647-49.
320) A. I. S. Kemp et al., “Episodic Growth of the Gondwana Supercontinent from Hafnium and Oxygen Isotopes in Zircon,” Nature 439 (2006): 580-583.
321) S. Tachibana et al., “60Fe in Chondrites: Debris from a Nearby Supernova in the Early Solar System?” Astrophysical Jour- nal 639 (2006): L87-90.
322) Koichiro Umemoto, Renata M. Wentzcovitch, and Philip B. Allen, “Dissociation of MgSiO3 in the Cores of Gas Giants and Terrestrial Exoplanets,” Science 311 (2006): 983-986.
323) Martin Kennedy et al., “Late Precambrian Oxygenation; Inception of the Clay Mineral Factory,” Science 311 (2006): 1446- 49.
324) Antony A. Stark and Youngung Lee, “Giant Molecular Clouds are More Concentrated Toward Spiral Arms than Smaller Clouds,” Astrophysical Journal 641 (2006): L113-116.
325) Mark A. Jensen et al., “Modeling the Role of Bacteriophage in the Control of Cholera Outbreaks,” Proceedings of the Na- tional Academy of Sciences, USA103 (2006): 4652-57.
326) C. L. Dobbs and I. A. Bonnell, “Spurs and Feathering in Spiral Galaxies,” Monthly Notices of the Royal Astronomical So- ciety 367 (2006): 873-878.
327) Gaspar Galaz et al., “Bulge Evolution in Face-on Spiral and Low Surface Brightness Galaxies,” Astronomical Journal 131 (2006): 2035-2049.
328) Martin D. Weinberg and Leo Blitz, “A Magellanic Origin for the Warp of the Galaxy,” Astrophysical Journal 641 (2006): L33-36.
329) Howie D. Scher and Ellen E. Martin, “Timing and Climatic Consequences of the Opening of Drake Passage,” Science 312 (2006): 428-30.
330) Armen Atoyan, James Buckley, and Henric Krawczynski, “A Gamma-Ray Burst Remnant in Our Galaxy: HESS J1303- 631,” Astrophysical Journal 642 (2006): L153-156.
331) M. Sol Alonso et al., “Effects of Galaxy Interactions in Different Environments,” Monthly Notices of the Royal Astronomi- cal Society 367 (2006): 1029-1038.
332) Keiichi Wada, Eiichiro Kokubo, and Junichiro Makino, “High-Resolution Simulations of a Moon-Forming Impact and Post-Impasct Evolution,” Astrophysical Journal 638 (2006): 1180-1186.
333) Daniel Rosenfeld, “Aerosols, Clouds, and Climate,” Science 312 (2006): 1323-24.
334) Steven Ian Dutch, “The Earth Has a Future,” Geosphere 2 (2006): 113-24.
335) J. Stuart B. Wyithe and Abraham Loeb, “Suppression of Dwarf Galaxy Formation by Cosmic Reionization,” Nature 441 (2006): 322-324.
336) Douglas G. Capone et al., “Follow the Nitrogen,” Science 312 (2006): 708-09.
337) Sean N. Raymond, “The Search for Other Earths: Limits on the Giant Planet Orbits That Allow Habitable Terrestrial Plan- ets to Form,” Astrophysical Journal 643 (2006): L131-134.
338) Catherine Constable and Monika Korte, “Is Earth’s Magnetic Field Reversing?” Earth and Planetary Science Letters 246 (2006): 1-16.
339) Sarah E. Robinson et al., “Silicon and Nickel Enrichment in Planet Host Stars: Observations and Implications for the Core Accretion Theory of Planet Formation,” Astrophysical Journal 643 (2006): 484-500.
340) Jan Bernkopf and Klaus Fuhrmann, “Local Subgiants and Time-scales of Disc Formation,” Monthly Notices of the Royal Astronomical Society 369 (2006): 673-676.
341) Christophe Lovis et al., “An Extrasolar Planetary System with Three Neptune-Mass Planets,” Nature 441 (2006): 305-309.
342) Richard A. Kerr, “Creatures Great and Small Are Stirring the Ocean,” Science 313 (2006): 1717.
343) Eric Kunze, et al, “Observations of Biologically Generated Turbulence in a Coastal Inlet,” Science 313 (2006): 1768-1770.
344) J. P. D. Abbatt, et al, “Solid Ammonium Sulfate Aerosols as Ice Nuclei: A Pathway for Cirrus Cloud Formation,” Science 313 (2006): 1770-1773,
345) James F. Kasting, “Ups and Downs of Ancient Oxygen,” Nature 443 (2006): 443-444.
346) Colin Goldblatt, Timothy M. Lenton, and Andrew J. Watson, “Bistability of Atmospheric Oxygen and the Great Oxida- tion,” Nature, 443 (2006): 683-686.
347) Rahul Shetty and Eve C. Ostriker, “Global Modeling of Spur Formation in Spiral Galaxies,” Astrophysical Journal 647 (2006): 997-1017.
348) Sean N. Raymond, et al, “Exotic Earths: Forming Habitable worlds with Giant Planet Migration,” Science 313 (2006): 1413-1416.
349) Takeshi Oka, “Interstellar H3+,” Proceedings of the National Academy of Sciences, vol. 103, no. 33 (2006): 12235-12242.
350) Andrea P. Buccino, Guillermo A. Lemarchand, and Pablo J. D. Mauas, “Ultraviolet Radiation Constraints Around the Cir- cumstellar Habitable Zones,” Icarus 183 (2006): 491-503.
351) Anatoly K. Pavlov et al., “Interstellar Gas Clouds and Planetary Habitability,” Astrobiology 6 (2006): 110-111.
352) Ing-Guey Jiang and Li-Chin Yeh, “On the Chaotic Orbits of Disk-Star-Planet Systems,” Astronomical Journal 128 (2004): 923-932.
353) Ross S. Stein, “Tidal Triggering Caught in the Act,” Science 305 (2004): 1248-1249.
354) S. Tanaka, M. Ohtake, and H. Sato, “Tidal Triggering of Earthquakes in Japan Related to Regional Tectonic Stress,” Earth, Planets, and Space 56 (2004):511-515.
355) Elizabeth S. Cochran, John E. Vidale, and Sachiko Tanaka, “Earth Tides Can Trigger Shallow Thrust Fault Earthquakes,” Science 306 (2004): 1164-1166.
356) Lucas J.Lourens, et al, “Astronomical Pacing of Late Palaeocene to Early Eocene Global Warming Events,” Nature 435 (2005): 1083-1087.
357) Richard A. Kerr, “Threshold Crossed on the Way to a Geodynamo in a Computer,” Science 309 (2005): 364-365.
358) Futoshi Takahashi, Masaki Matsushima, Yoshimori Honkura, “Simulations of a Quasi-Taylor State Geomagnetic Field in- cluding Polarity Reversals on the Earth Simulator,” Science 309 (2005): 459-461.
359) David C. Catling, et al, “Why O2 Is Required by Complex Life on Habitable Planets and the Concept of Planetary “Oxy- genation Tine,” Astrobiology 5 (2005): 415-438.
360) Fred J. Ciesla and Jeffrey N. Cuzzi, “The Distribution of Water in Protoplanetary Disks,” Astrobiology 6 (2006): 120.
361) Alexander A. Pavlov, Owen B. Toon, and Tian Feng, “Methane Runaway in the Early Atmosphere – Two Stable Climate States of the Achean?,” Astrobiology 6 (2006): 161.
362) Richard A. Kerr, “Hunt for Birthplace of Meteorites Yields New View of Earth’s Origins,” Science 311 (2006): 932.
363) Kenji Bekki et al., “Cluster Cannibalism and Scaling Relations of Galactic Stellar Nuclei,” The Astrophysical Journal Let- ters 610 (2004): L13-L16.
364) D. J. Pisano et al., “Where are the High-Velocity Clouds in Local Group Analogs?” The Astrophysical Journal Letters 610 (2004): L17-L20.
365) S. Cazaux and M. Spaans, “Molecular Hydrogen Formation on Dust Grains in the High-Redshift Universe,” The Astro- physical Journal 611 (2004): 40-51.
366) Sergey Mashchenko and Alison Sills , “Globular Clusters with Dark Matter Halos. I. Initial Relaxation,” The Astrophysical Journal 619 (2005): 243-257.
367) Sergey Mashchenko and Alison Sills, “Globular Clusters with Dark Matters Halos. II. Evolution in a Tidal Field ,” The As- trophysical Journal 619 (2005): 258-269.
368) R. J. Wilman et al., “The Discovery of a Galaxy-Wide Superwind from a Young Massive Galaxy at Redshift z ≈ 3,” Nature 436 (2005): 227-229.
369) Chris B. Brook et al., “The Emergence of the Thick Disk in a CDM Universe. II. Colors and Abundance Patterns,” The As- trophysical Journal 630 (2005): 298-308.
370) S. Savaglio et al., “The Gemini Deep Deep Survey. VII. The Redshift Evolution of the Mass-Metallicity Relation,” The As- trophysical Journal 635 (2005): 260-279.
371) Chris B. Brook et al., “Disk Evolution Since z ~ 1 in a CDM Universe,” The Astrophysical Journal 639 (2006): 126-135.
372) Masataka Fukugita and P. J. E. Peebles, “Massive Coronae of Galaxies,” The Astrophysical Journal 639 (2006): 590-599.
373) C. Maier et al., “Oxygen Gas Abundances at z ~ 1.4: Implications for the Chemical Evolution History of Galaxies,” The As- trophysical Journal 639 (2006): 858-867.
374) Yuexing Li et al., “Star Formation in Isolated Disk Galaxies. II. Schmidt Laws and Efficient of Gravitational Collapse,” The Astrophysical Journal 639 (2006): 879-896.
375) D. B. Zucker, “A New Milky Way Dwarf Satellite in Canes Venatici,” The Astrophysical Journal 643 (2006): L103-L106.
376) Jesper Sommer-Larsen, “Where are the ‘Missing’ Galactic Baryons?,” The Astrophysical Journal Letters 644 (2006): L1- L4.
377) Brant Robertson et al., “A Merger-Driven Scenario for Cosmological Disk Galaxy Formation,” The Astrophysical Journal 645 (2006): 986-1000.
378) Yeshe Fenner et al., “Cosmological Implications of Dwarf Spheroidal Chemical Evolution,” The Astrophysical Journal 646 (2006): 184-191.
379) C. P. Haines et al., “The Different Environmental Dependencies of Star Formation for Giant and Dwarf Galaxies,” The As- trophysical Journal 647 (2006): L21-L24.
380) Sadegh Khochfar and Joseph Silk, “A Simple Model for the Size Evolution of Elliptical Galaxies,” The Astrophysical Journal Letters 648 (2006): L21-L24.
381) D. J. Hanish et al., “The Survey for Ionization in Neutral Gas Galaxies. II. The Star Formation Rate Density of the Local Universe,” The Astrophysical Journal 649 (2006): 150-162.
382) Ignacio Trubillo et al., “The Size Evolution of Galaxies Since z~3: Combining SDSS, GEMS, and FIRES,” The Astro- physical Journal 650 (2006): 18-41.
383) D. B. Zucker et al., “A Curious Milky Way Satellite in Ursa Major,” The Astrophysical Journal Letters 650 (2006): L41- L44.
384) Misty A. La Vigne, Stuart N. Vogel and Eve C. Ostriker, “A Hubble Space Telescope Archival Survey of Feathers in Spiral Galaxies,” The Astrophysical Journal 650 (2006): 818-834.
385) D. R. Gies and J. W. Helsel, “Ice Age Epochs and the Sun’s Path Through the Galaxy,” The Astrophysical Journal 626 (2005): 844-848.
386) Sun Kwok, “The Synthesis of Organic and Inorganic Compounds in Evolved Stars,” Nature 430 (2004): 985-991.
387) Ignasi Ribas et al., “Evolution of the Solar Activity Over Time and Effects on Planetary Atmospheres. I. High-Energy Irra- diances (1-1700 Å),” The Astrophysical Journal 622 (2005): 680-694.
388) Rupali Chandar, Bradley Whitmore, and Myung Gyoon Lee, “The Globular Cluster Systems of Five Nearby Spiral Galax- ies: New Insights from Hubble Space Telescope Imaging,” The Astrophysical Journal 611 (2004): 220-244.
389) Daniel B. Zucker et al., “Andromeda IX: A New Dwarf Spheroidal Satellite of M31,” The Astrophysical Journal Letters 612 (2004): L121-L124.
390) Katharina Lodders, “Jupiter Formed with More Tar Than Ice,” The Astrophysical Journal 611 (2004): 587-597.
391) Soko Matsumura and Ralph E. Pudritz, “Dead Zones and the Origin of Planetary Masses,” The Astrophysical Journal Let- ters 618 (2005): L137-L140.
392) Roman R. Rafikov, “Can Giant Planets Form by Direct Gravitational Instability?,” The Astrophysical Journal Letters 621 (2005): L69-L72.
393) Alan P. Boss , “Evolution of the Solar Nebula. VII. Formation and Survival of Protoplanets Formed by Disk Instability,” The Astrophysical Journal 629 (2005): 535-548.
394) Thayne Currie , “Hybrid Mechanisms for Gas/Ice Giant Planet Formation,” The Astrophysical Journal 629 (2005): 549- 555.
395) Kai Cai et al., “The Effects of Metallicity and Grain Size on Gravitational Instabilities in Protoplanetary Disks,” The Astro- physical Journal Letters 636 (2006): L149-L152.
396) M. Lecar et al., “On the Location of the Snow Line in a Protoplanetary Disk,” The Astrophysical Journal 640 (2006): 1115- 1118.
397) Bernard Marty, “The Primordial Porridge,” Science 312 (2006): 706-707.
398) Henner Busemann et al., “Interstellar Chemistry Recorded in Organic Matter from Primitive Meteorites,” Science 312 (2006): 727-730.
399) A. B. Verchovsky, I. P. Wright, and C. T. Pillinger, “Astrophysical Significance of Asymptotic Giant Branch Stellar Wind Energies Recorded in Meteoritic SiC Grains,” The Astrophysical Journal 607 (2004): 611-619.
400) J. Jeff Hester et al., “The Cradle of the Solar System,” Science 304 (2004): 1116-1117.
401) Julianne J. Dalcanton and Peter Yoachim, “The Formation of Dust Lanes: Implications for Galaxy Evolution,” The Astro- physical Journal 608 (2004): 189-207.
402) Andrey V. Kravtsov, Oleg Y Gnedin, and Anatoly A. Klypin, “The Tumultuous Lives of Galactic Dwarfs and the Missing Satellites Problem,” The Astrophysical Journal 609 (2004): 482-497.
403) J. Trujillo Bueno, N. Shchukina, and A. Asensio Ramos, “A Substantial Amount of Hidden Magnetic Energy in a Quiet Sun,” Nature 430 (2004): 326-329.
404) Masahiro Nagashima and Yuzuru Yoshi, “Hierarchical Formation of Galaxies with Dynamical Response to Supernova- Induced Gas Removal,” The Astrophysical Journal 610 (2004): 23-44.
405) Krystal Tyler et al., “Diffuse X-Ray Emission in Spiral Galaxies,” The Astrophysical Journal 610 (2004): 213-225.
406) Stuart Ross Taylor, “Why Can’t Planets be Like Stars,” Nature 430 (2004): 509.
407) Bart De Pontieu, Robert Edelyi, and Stewart P. James, “Solar Chromospheric Spicules from the Leakage of Photospheric Oscillations and Flows,” Nature 430 (2004): 536-539.
408) Jordi José et al., “The Imprint of Nova Nucleosynthesis in Presolar Grains,” The Astrophysical Journal 612 (2004): 414- 428.
409) Gregory Laughlin, Peter Bodenheimer, and Fred C. Adams, “The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs,” The Astrophysical Journal Letters 612 (2004): L73-L76.
410) Smail Mostefaoui and Peter Hoppe, “Discovery of Abundant in Situ Silicate and Spinel Grains from Red Giant Stars in a Primitive Meteorite,” The Astrophysical Journal Letters 613 (2004): L149-L152.
411) F. A. Aharonian et al., “High-energy Particle Acceleration in the Shell of a Supernova Remnant,” Nature 432 (2004): 75- 77.
412) Daniel Clery, “Hot on the Trail of Cosmic Rays,” Science 306 (2004): 956.
413) Jennifer Simmerer et al., “The Rise of the s-Process in the Galaxy,” The Astrophysical Journal 617 (2004): 1091-1114.
414) G. C. Jordan IV and B. S. Meyer, “Nucleosynthesis in Fast Expansions of High-Entropy, Proton-Rich Matter,” The Astro- physical Journal Letters 617 (2004): L131-L134..
415) B. R. McNamara et al., “The Heating of Gas in a Galaxy Cluster by X-ray Cavities and Large-Scale Shock Fronts,” Nature 433 (2005): 45-47.
416) Stéphanie Juneau et al., “Cosmic Star Formation History and its Dependence on Galaxy Stellar Mass,” The Astrophysical Journal Letters 619 (2005): L135-L138.
417) Tiziana Di Matteo, Voker Springel, and Lars Hernquist, “Energy Input from Quasars Regulates the Growth and Activity of Black Holes and Their Host Galaxies,” Nature 433 (2005): 604-607.
418) W. H. Baumgartner et al., “Intermediate-Element Abundances in Galaxy Clusters,” The Astrophysical Journal 620 (2005): 680-696.
419) Dimitri Veras and Philip J. Armitage, “The Influence of Massive Planet Scattering on Nascent Terrestrial Planets,” The As- trophysical Journal Letters 620 (2005): L111-L114.
420) Artashes Petrosian et al., “Active and Star-Forming Galaxies and Their Supernovae,” The Astronomical Journal 129 (2005): 1369-1380.
421) Debra A. Fischer and Jeff Valenti, “The Planet-Metallicity Correlation,” The Astrophysical Journal 622 (2005): 1102- 1117.
422) David W. Hogg et al., “Mid-Infrared and Visible Photometry of Galaxies: Anomalously Low Polycyclic Aromatic Hydro- carbon Emission from Low-Luminosity Galaxies,” The Astrophysical Journal 624 (2005): 162-167.
423) A. C. Quillen and Ivan Minchev, “The Effect of Spiral Structure on the Stellar Velocity Distribution in the Solar Neighbor- hood,” The Astronomical Journal 130 (2005): 576-585.
424) Massimo Ricotti and Nickolay Y. Gnedin, “Formation Histories of Dwarf Galaxies in the Local Group,” The Astrophysical Journal 629 (2005): 259-267.
425) Guy Worthey et al., “M31’s Heavy-Element Distribution and Outer Disk,” The Astrophysical Journal 631 (2005): 820-831.
426) Stefi Baum et al., “Hubble Space Telescope STIS Spectroscopy of the Lyα Emission Line in the Central Dominant Galax- ies in A426, A1795, and A2597: Constraints on Clouds in the Intracluster Medium,” The Astrophysical Journal 632 (2005): 122-136.
427) Jinyoung Serena Kim et al., “Formation and Evolution of Planetary Systems Cold Outer Disks Associated with Sun-Like Stars,” The Astrophysical Journal 632 (2005): 659-669..
428) Sean N. Raymond et al., “Terrestrial Planet Formation in Disks with Varying Surface Density Profiles,” The Astrophysical Journal 632 (2005): 670-676.
429) Scott C. Chapman et al., “A Keck Deimos Kinematic Study of Andromeda IX: Dark Matter on the Smallest Galactic Scales,” The Astrophysical Journal Letters 632 (2005): L87-L90.
430) Jeremy R. King, Ann M. Boesgaard, and Simon Schuler, “Keck Hires Spectroscopy of Four Candidate Solar Twins,” The Astronomical Journal 130 (2005): 2318-2325.
431) Joseph M. Hahn and Renu Malhotra, “Neptune’s Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simu- lations to Observations,” The Astronomical Journal 130 (2005): 2392-2414.
432) M. Mouhcine et al., “Halos of Spiral Galaxies. II. Halo Metallicity-Luminosity Relation,” The Astrophysical Journal 633 (2005): 821-827.
433) M. Mouhcine et al., “Halos of Spiral Galaxies. III. Metallicity Distributions,” The Astrophysical Journal 633 (2005): 828- 843.
434) Douglas McNeil, Martin Duncan, and Harold F. Levison, “Effects of Type I Migration on Terrestrial Planet Formation,” The Astronomical Journal 130 (2005): 2884-2899.
435) A. Ecuvillon, et al, “Oxygen Abundances in Planet-Harboring Stars: Comparison of Different Abundance Indicators,” As- tronomy & Astrophysics, 445 (2006): 633-645.
436) M. Haverkorn et al., “Enhanced Small-Scale Faraday Rotation in the Galactic Spiral Arms,” The Astrophysical Journal Letters 637 (2006): L33-L35.
437) Fred J. Ciesla and Jeffrey N. Cuzzi, “The Distribution of Water in Protoplanetary Disks,” Astrobiology 6 (2006): 120.
438) Lynn J. Rothschild, “The Role of the Moon in Shaping Life on Earth,” Astrobiology 6 (2006): 123.
439) Nathan Kaib and Tom Quinn, “The Effect of the Sun’s Early Environment on the Oort Cloud and Comet Showers,” Astro- biology 6 (2006): 247.
440) Marc J. Kuchner and Sara Seager, “Extrasolar Carbon Planets,” Astrobiology 6 (2006): 274.
441) A. Higuchi and E. Kokubo, “Scattering of Planetesimals by a Planet: Formation of Comet Cloud Candidates,” The Astro- nomical Journal 131 (2006): 1119-1129.
442) J. E. Chiar and A. G. G. M. Tielens, “Pixie Dust: The Silicate Features in the Diffuse Interstellar Medium,” The Astro- physical Journal 637 (2006): 774-785.
443) Kenji Bekki and Masashi Chiba, “Impact of Dark Matter Subhalos on Extended H I Disks of Galaxies: Possible Formation of H I Fine Structures and Stars,” The Astrophysical Journal Letters 637 (2006): L97-L100.
444) Alan P. Boss, “On the Formation of Gas Giant Planets on Wide Orbits,” The Astrophysical Journal Letters 637 (2006): L137-L140.
445) Rory Barnes and Richard Greenberg, “Extrasolar Planetary Systems Near a Secular Separatrix,” The Astrophysical Journal 638 (2006): 478-487.
446) Alison L. Coil et al., “The Deep2 Galaxy Redshift Survey: Redshift Survey: Clustering of Groups and Group Galaxies at z~1,” The Astrophysical Journal 638 (2006): 668-685.
447) Keichi Wada, Eiichiro Kokubo, and Junichiro Makino, “High-Resolution Simulations of a Moon-Forming Impact and Postimpact Evolution,” The Astrophysical Journal 638 (2006): 1180-1186.
448) Lawrence R. Mudryk and Yanqin Wu, “Resonance Overlap is Responsible for Ejecting Planets in Binary Systems,” The Astrophysical Journal 639 (2006): 423-431.
449) Guangtun Zhu et al., “The Dependence of the Occupation of Galaxies on the Halo Formation Time,” The Astrophysical Journal Letters 639 (2006): L5-L8.
450) Xiaohu Yang, H. J. Mo, and Frank C. van den Bosch, “Observational Evidence for an Age Dependence of Halo Bias,” The Astrophysical Journal Letters 638 (2006): L55-L58.
451) Rosemary F. G. Wyse, “Further Evidence of a Merger Origin for the Thick Disk: Galactic Stars Along Lines of Sight to Dwarf Spheroidal Galaxies,” The Astrophysical Journal Letters 639 (2006): L13-L16.
452) S. Tachibana et al., “60Fe in Chondrites: Debris from a Nearby Supernova in the Early Solar System,” The Astrophysical Journal Letters 639 (2006): L87-L90.
453) Weibiao Hsu et al., “A Late Episode of Irradiation in the Early Solar System: Evidence from Extinct 36C1 and 26A1 in Meteorites,” The Astrophysical Journal 640 (2006): 525-529.
454) Takeru K. Suzuki, “Forecasting Solar Wind Speeds,” The Astrophysical Journal Letters 640 (2006): L75-L78.
455) Gaspar Galaz, Alvaro Villalobos, and Leopoldo Infante, “Bulge Evolution in Face-On Spiral and Low Surface Brightness Galaxies,” The Astrophysical Journal 131 (2006): 2035-2049.
456) Alessandro Sozzetti et al., “Chemical Composition of the Planet-Harboring Star TrES-1,” The Astronomical Journal 131 (2006): 2274-2289.
457) S. C. Glover, “Cosmological Implications of the Uncertainty in H- Destruction Rate Coefficients,” The Astrophysical Jour- nal 640 (2006): 553-568.
458) Daniel Grether and Charles H. Lineweaver, “How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions Around Nearby Sun-Like Stars,” The Astrophysical Journal 640 (2006): 1051-1062.
459) John M. Fregeau, Sourav Chatterjee, and Frederick A. Rasio, “Dynamical Interactions of Planetary Systems in Dense Stel- lar Environments,” The Astrophysical Journal 640 (2006): 1086-1098.
460) P. Variére et al., “Planets Rapidly Create Holes in Young Circumstellar Disks,” The Astrophysical Journal 640 (2006): 1110-1114.
461) P. Variére et al., “Planets Rapidly Create Holes in Young Circumstellar Disks,” The Astrophysical Journal 640 (2006): 1110-1114.
462) B. O’Halloran, S. Satyapal, and R. P. Dudik, “The Polycyclic Aromatic Hydrocarbon Emission Deficity in Low-Metallicity Galaxies – A Spitzer View,” The Astrophysical Journal 641 (2006): 795-800.
463) Bianca M. Poggianti et al., “The Evolution of the Star Formation Activity in Galaxies and its Dependence on Environ- ment,” The Astrophysical Journal 642 (2006): 188-215.
464) F. Shankar et al., “New Relationships Between Galaxy Properties and Host Halo Mass, and the Role of Feedbacks in Gal- axy Formation,” The Astrophysical Journal 643 (2006): 14-25.
465) Sarah E. Robinson et al., “Silicon and Nickel Enrichment in Planet Host Stars: Observations and Implications for the Core Accretion Theory of Planet Formation,” The Astrophysical Journal 643 (2006): 484-500.
466) A. S. Fruchter et al., “Long γ-Ray Bursts and Core-Collapse Supernovae Have Different Environments,” Nature 463 (2006): 463-468.
467) R. Earle Luck and Ulrike Hetter, “Dwarfs in the Local Region,” The Astronomical Journal 131 (2006): 3069-3092.
468) Alan P. Boss, “Rapid Formation of Super-Earths around M Dwarf Stars,” The Astrophysical Journal Letters 644 (2006): L79-L82.
469) Joseph A. Nuth III et al., “A Mechanism for the Equilibrium Growth of Mineral Crystals in AGB Stars and Red Gians on 105 yr Timescales,” The Astrophysical Journal 644 (2006): 1164-1170.
470) Christopher J. Burke et al., “Survey for Transiting Extrasolar Planets in Stellar Systems. III. A Limit on the Fraction of Stars with Planets in the Open Cluster NGC 1245,” The Astronomical Journal 132 (2006): 210-230.
471) James J, Wray, et al, “The Shape, Multiplicity, and Evolution of Superclusters in ËCDM Cosmology,” Astrophysical Journal, 652 (2006): 907-916.
472) M. M. Romanova and R. V. E. Lovelace, “The Magnetospheric Gap and the Accumulation of Giant Planets Close to a Star,” The Astrophysical Journal Letters 645 (2006): L73-L76.
473) Francisco Prada et al., “How Far Do They Go? The Outer Structure of Galactic Dark Matter Halos,” The Astrophysical Journal 645 (2006): 1001-1011.
474) Paul O. Wennberg, “Atmospheric Chemistry: Radicals Follow the Sun,” Nature 442 (2006): 145-146.
475) Franz Rohrer and Harald Berresheim, “Strong Correlation Between Levels of Tropospheric Hydroxyl Radicals and Solar Ultraviolet Radiation,” Nature 442 (2006): 184-187.
476) R. P. Butler et al., “Catalog of Nearby Exoplanets,” The Astrophysical Journal 646 (2006): 505-522.
477) Woong-Tae Kim and Eve C. Ostriker, “Formation of Spiral-Arm Spurs and Bound Clouds in Vertically Stratified Galactic Gas Disks,” The Astrophysical Journal 646 (2006): 213-231.
478) R. E. Luck, V. V. Kovtyukh, and S. M. Andrievsky, “The Distribution of Elements in the Galactic Disk,” The Astronomical Journal 132 (2006): 902-918.
479) Andreea S. Font et al., “Phase-Space Distributions of Chemical Abundances in Milky Way-Type Galaxy Halos,” The As- trophysical Journal 646 (2006): 886-898.
480) Brian A. Keeney et al., “Does the Milky Way Produce a Nuclear Galactic Wind?,” The Astrophysical Journal 646 (2006): 951-964.
481) Christopher L. Fryer et al., “Supernova Fallback: A Possible Site for the r-Process,” The Astrophysical Journal Letters 646 (2006): L131-L134.
482) Krzysztof Goździewski and Maciej Konacki, “Trojan Pairs in the HD 128311 and HD 82943 Planetary Systems?” The Astrophysical Journal 647 (2006): 573-586.
483) Katharina Lodders, “They Came from the Deep in the Supernova: The Origin of TiC and Metal Subgrains in Presolar Graphite Grains,” The Astrophysical Journal Letters 647 (2006): L37-L40.
484) Ariyeh H. Maller, “Galaxy Merger Statistics and Inferred Bulge-to-Disk Ratios in Cosmological SPH Simulations,” The Astrophysical Journal 647 (2006): 763-772.
485) Rahul Shetty and Eve C. Ostriker, “Global Modeling of Spur Formation in Spiral Galaxies,” The Astrophysical Journal 647 (2006): 997-1017.
486) Kevin Schawinski et al., “Suppression of Star Formation in Early-Type Galaxies by Feedback from Supermassive Black Holes,” Nature 442 (2006): 888-891.
487) Masahiro Ikoma, “Constraints on the Mass of a Habitable Planet with Water of Nebular Origin,” The Astrophysical Journal 648 (2006): 696-706.
488) Gajendra Pandey, “The Discovery of Fluorine in Cool Extreme Helium Stars,” The Astrophysical Journal 648 (2006): L143-L146.
489) Richard A. Kerr, “Has Lazy Mixing Spoiled the Primordial Stew?” Science 314 (2006): 36-37.
490) Grant M. Kennedy, Scott J. Kenyon and Benjamin C. Bromley, “Planet Formation Around Low-Mass Stars: The Moving Snow Line and Super-Earths,” The Astrophysical Journal 650 (2006): L139-L142.
491) Richard A. Kerr, “The Kuiper Belt Loses Some of Its Mystery,” Science 314 (2006): 590.
492) Pavel a. Denissenkov, Marc Pinsonneault and Donald M. Terndrup, “Fluorine Abundance Variations as a Signature of Enhanced Extra Mixing in Red Giants of the Globular Cluster,” The Astrophysical Journal 651 (2006): 438-443.
493) Eric F. Bell et al., “The Merger Rate of Massive Galaxies,” The Astrophysical Journal 652 (2006): 270-276.
494) Gennard D’Angelo, Stephen H. Lubow and Matthew R. Bate, “Evolution of Giant Planets in Eccentric Risks,” The Astrophysical Journal 652 (2006): 1698-1714.
495) Leslie W. Looney, John J. Tobin and Brian D. Fields, “Radioactive Probes of the Supernova-Contaminated Solar Nebula: Evidence That the Sun Was Born in a Cluster,” The Astrophysical Journal 652 (2006): 1755-1762.
496) J. E. Chambers, “Planet Formation with Migration,” The Astrophysical Journal Letters 652 (2006): L133-L136.
497) A. Cimatti et al., “Old Galaxies in the Young Universe,” Nature 430 (2004): 184-187.
498) P. Colín et al., “Dwarf Dark Matter Halos,” The Astrophysical Journal 612 (2004): 50-57.
499) Akima Fujita et al., “Cosmological Feedback from High-Redshift Dwarf Galaxies,” The Astrophysical Journal 613 (2004): 159-179.
500) Weike Xiao, Zhengfan Sun, and Heng Hao, “A Physical Bias in Cosmological Simulations,” The Astrophysical Journal Letters 617 (2004): L103-L106.
501) Anna Pasquali et al., “Discovery of a Solitary Dwarf Galaxy in the Apples Survey,” The Astronomical Journal 129 (2005): 148-159.
502) Varsha Kukarni et al., “Hubble Space Telescope Observations of Element Abundances in Low-Redshift Damped Lyα Galaxies and Implications for the Global Metallicity-Redshift Relation,” The Astrophysical Journal 618 (2005): 68-90.
503) Critiano Porciana and Piero Madau, “The Origin of Intergalactic Metals Around Lyman Break Galaxies,” The Astrophysical Journal Letters 625 (2005): L43-L46.
504) R. J. Wilman et al., “The Discovery of a Galaxy-Wide Superwind from a Young Massive Galaxy at Redshift z ≈ 3,” Nature 436 (2005): 227-229.
505) C. Simon Jeffery, Christopher A. Tout, John C. Lattanzio, “Nucleosynthesis in Binary Stars,” Science 311 (2006): 345-346.
506) Ben E. K. Sugerman et al., “Massive-Star Supernovae as Major Dust Factories,” Science Express, 10.1126/science.1128131 (2006).,” Science 309 (2006): 1431.
507) J. Pruet and R. D. Hoffman, “Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos,” The Astrophysical Journal 644 (2006): 1028-1039.
508) Ignacio Trubillo et al., “The Size Evolution of Galaxies Since z~3: Combining SDSS, GEMS, and FIRES,” The Astrophysical Journal 650 (2006): 18-41.
509) S. Dye and S. J. Warren, “Decomposition of the Visible and Dark Matter in the Einstein Ring 0047-2808 by Semilinear In- version,” The Astrophysical Journal 623 (2005): 31-41.
510) Sergey Mashchenko, H. M. P. Couchman, and Alison Sills , “Modeling Star Formation in Dwarf Spheroidal Galaxies: A Case for Extended Dark Matter Halos,” The Astrophysical Journal 624 (2005): 726-741.
511) Andreea Petric et al., “A Direct Upper Limit on the Density of Cosmological Dust from the Absence of an X-Ray Scattering Halo Around the z = 4.3 Quasar QSO 1508+5714,” The Astrophysical Journal 651 (2006): 41-45.
512) M. S. del Río, E. Brinks and J. Cepa, “High-Resolution H I Observations of the Galaxy NGC 404: A Dwarf S0 with Abundant Interstellar Gas,” The Astronomical Journal 128 (2004): 89-102.
513) Xiao Wang et al., “Estimating Dark Matter Distributions,” The Astrophysical Journal 626 (2005): 145-158.
514) Georg Feulner et al., “Specific Star Formation Rates to Redshift 5 from the FORS Deep Field and the GOOD-S Field,” The Astrophysical Journal Letters 633 (2005): L9-L12.
515) Charlie Conroy et al., “The Deep2 Galaxy Redshift Survey: Probing the Evolution of Dark Matter Halos Around Isolated Galaxies from z ~ 1 to z ~ 0,” The Astrophysical Journal 635 (2005): 982-989.
516) Juna A. Kollmeier et al., “Galactic Wind Effects on the Lyα Absorption in the Vicinity of Galaxies,” The Astrophysical Journal 638 (2006): 52-71.
517) F. D. A. Hartwick, “Early Cosmic Chemical Evolution: Relating the Origin of a Diffuse Intergalactic Medium and the First Long-Lived Stars,” The Astrophysical Journal 640 (2006): 41-46.
518) Tim W. Connors et al., “On the Origins of Anomalous Velocity Clouds in the Milky Way,” The Astrophysical Journal 646 (2006): L53-L56.
519) F. W. Stecker, M. A. Malkan and S. T. Scully, “Intergalactic Photon Spectra from the Far-IR to the UV Lyman Limit for 0 < z < 6 and the Optical Depth of the Universe to the High-Energy Gamma Rays,” The Astrophysical Journal 648 (2006): 774-783.
520) Jorge A. Vasquez and Mary R. Reid, “Probing the Accumulation History of the Voluminous Toba Magma,” Science 305 (2004): 991-994.
521) P. C. Tzedakis et al., “The Duration of Forest Stages in Southern Europe and Interglacial Climate Variability,” Science 306 (2004): 2231-2235.
522) Gerald H. Haug et al., “North Pacific Seasonality and the Glaciation of North America 2.7 Million Years Ago,” Nature 433 (2005): 821-825.
523) Richard A. Kerr, “Looking Way Back for the World’s Climate Future,” Science 312 (2006): 1456-1457.
524) A. V. Fedorov et al., “The Pliocene Paradox (Mechanisms for a Permanent El Niño),” Science 312 (2006): 1485-1489.
525) Joyce E. Penner, Xiquan Dong, and Yang Chen, “Observational Evidence of a Change in Radiative Forcing Due to the Indirect Aerosol Effect,” Nature 427 (2004): 231-234.
526) Joyce E. Penner, “The Cloud Conundrum,” Nature 432 (2004): 962-963.
527) Andrew S. Ackerman et al., “The Impact of Humidity Above Stratiform Clouds on Indirect Aerosol Climate Forcing,” Nature 432 (2004): 1014-1017.
528) Jim Coakley, “Atmosphere Physics: Reflections on Aerosol Cooling,” Nature 438 (2005): 1091-1092.
529) Nicolas Bellouin et al., “Global Estimate of Aerosol Direct Radiative Forcing from Satellite Measurements,” Nature 438 (2005): 1138-1141.
530) Richard D. Bardgett et al., “Parasitic Plants Indirectly Regulate Below-Ground Properties in Grassland Ecosystems,” Nature 439 (2006): 969-972.
531) Louis A. Derry, “Fungi, Weathering, and the Emergence of Animals,” Science 311 (2006): 1386-1387.
532) Martin Kennedy et al., “Late Precambrian Oxygenation: Inception of the Clay Mineral Factory,” Science 311 (2006): 1446- 1449.
533) Edward F. DeLong, “Microbial Life Breathes Deep,” Science 306 (2004): 2198-2200.
534) Steven D’Hondt et al., “Distributions of Microbial Activities in Deep Subseafloor Sediments,” Science 306 (2004): 2216- 2220.
535) Bernard J. Wood, Michael J. Walter, and Jonathan Wade, “Accretion of the Earth and Segregation of Its Core,” Nature 441 (2006): 825-833.
536) Piero Di Carlo et al., “Missing OH Reactivity in a Forest: Evidence for Unknown Reactive Biogenic VOCs,” Science 304 (2004): 722-725.
537) S. Perkins, “It’s a Gas: Trees Emit Unknown Volatile Substances,” Science News 165 (2004): 277-278.
538) Jean-Pierre Valet, Laure Meynadier, and Yohan Guyodo, “Geomagnetic Dipole Strength and Reversal Rate Over the Past Two Million Years,” Nature 435 (2005): 802-805.
539) Shuichi Kodaira et al., “High Pore Fluid Pressure May Cause Silent Slip in the Nankai Trough,” Science 304 (2004): 1295- 1298.
540) G. N. Phillips and K. A. Evans, “Role of CO2 in the Formation of Gold Deposits,” Nature 429 (2004): 860-863.
541) K. G. Schulz et al., “Effect of Trace Metal Availability on Coccolithophorid calcification,” Nature 430 (2004): 673-676.
542) Randal D. Koster et al., “Regions of Strong Coupling Between Soil Moisture and Precipitation,” Science 305 (2004): 1138- 1140.
543) Körtzinger et al., “The Ocean Takes a Deep Breath,” Science 306 (2004): 1337.
544) Charles S. Hopkinson Jr. and Joseph J. Vallino, “Efficient Export of Carbon to the Deep Ocean through Dissolved Organic Matter,” Nature 433 (2005): 142-145.
545) Heide N. Schulz and Horst D. Schulz, “Large Sulfur Bacteria and the Formation of Phosphorite,” Science 307 (2005): 416- 417.
546) Torstein Berndt et al., “Rapid Formation of Sulfuric Acid Particles at Near-Atmospheric Conditions,” Science 307 (2005): 698-700.
547) Amitabh Avasthi, “Extinguished Earth,” ScienceNOW Daily News, 28 Jan 2005, (128):1; ScienceNOW 307 (2005): 639.
548) Louis A. Derry et al., “Biological Control of Terrestrial Silica Cycling and Export Fluxes to Watersheds,” Nature 433 (2005): 728-731.
549) Patrick Jöckel and Carl A. M. Brenninkmeijer, “Natural Bleach under Scrutiny,” Nature 436/18 (2005): 921-922.
550) Martin R. Manning et al., “Short-term Variations in the Oxidizing Power of the Atmosphere,” Nature 436/18 (2005): 1001- 1004.
551) Ashna A. Raghoebarsing et al., “Methanotrophic Symbionts Provide Carbon for Photosynthesis in Peat Bogs,” Nature 436 (2005): 1153-1156.
552) Ashna A. Raghoebarsing et al., “A Microbial Consortium Couples Anaerobic Methane Oxidation to Denitrification,” Na- ture 440 (2006): 918-921.
553) Curtis A. Suttle, “Viruses in the Sea,” Nature 437 (2005): 356-361.
554) David C. Lowe et al., “A Green Source of Surprise,” Nature 439 (2006): 148-149.
555) Alison Butler, “Microbial Iron Mobilization: New Marine Siderophores,” Astrobiology 6 (2006): 126.
556) Rajdeep Dasgupta and Marc Hirschmann, “Melting in the Earth’s Deep Upper Mantle Caused by Carbon Dioxide,” Nature 440 (2006): 659-662.
557) Peter B. Reich et al., “Nitrogen Limitation Constrains Sustainability of Ecosystem Response to CO2,” Nature 440 (2006): 922-925.
558) S. A. Goldthwait et al., “Effects of Physical Fragmentation on Remineralization of Marine Snow,” Marine Ecology Progress Series 305 (2005): 59-65.
559) Uta Passow, “There’s More to Marine Snow Than Meets the Eye,” Nature 440 (2006): 840.
560) Rudolf K. Thauer and Seigo Shima, “Methane and Microbes,” Nature 440 (2006): 878-879.
561) Peter B. Reich et al., “Nitrogen Limitation Constrains Sustainability of Ecosystem Response to CO2,” Nature 440 (2006): 922-925.
562) Alexander F. Goncharov, Viktor V. Struzhkin, and Steven D. Jacobsen, “Reduced Radiative Conductivity of Low-Spin (Mg,Fe)O in the Lower Mantle,” Science 312 (2006): 1205-1208.
563) Daniel Rosenfeld, “Aerosols, Clouds, and Climate,” Science 312 (2006): 1323-1324.
564) U. Dusek et al., “Size Matters More Than Chemistry for Cloud-Nucleating Ability of Aerosol Particles,” Science 312 (2006): 1375-1378.
565) Gill Malin, “New Pieces for the Marine Sulfur Cycle Jigsaw,” Science 314 (2006): 607-608.
566) Erinn C. Howard et al. Bacterial Taxa That Limit Sulfur Flux from the Ocean Science 314 2006 649-652.
567) Maria Vila-Costa et al. Dimethylsulfoniopropionate Uptake by Marine Phytoplankton Science 314 2006 652-654.
568) Nicholas Meskhidze and Athanasios Nenes, “Phytoplankton and Cloudiness in the Southern Ocean,” Science 314 (2006): 1419-1423.
569) Michael J. Behrenfeld et al., “Climate-Driven Trends in Contemporary Ocean Productivity,” Nature 444 (2006): 752-755.
570) Andrea P. Buccino, Guillermo A. Lemarchand, and Pablo J. D. Mauas, “Ultraviolet Radiation Constraints around the Cir- cumstellar Habitable Zones,” Icarus 183 (2006): 491-503.
571) François-Marie Bréon, “How Do Aerosols Affect Cloudiness and Climate?” Science 313 (2006): 623-624.
572) Paul Martini et al., “Spectroscopic Confirmation of a Large Population of Active Galactic Nuclei in Clusters of Galaxies,” Astrophysical Journal 644 (2006): 116-132.
573) C.M. Lisse et al., “Spitzer Spectral Observations of the Deep Impact Ejecta,” Science 313 (2006): 635-640.
574) Sergey Mashchenko, H. M. P. Couchman, and James Wadsley, “The Removal of Cusps from Galaxy Centres by Stellar Feedback in the Early Universe,” Nature 442 (2006): 539-542.
575) Sean N. Raymond, Avi M. Mandell, and Steinn Sigurdsson, “Exotic Earths: Forming Habitable Worlds with Giant Planet Migration,” Science 313 (2006): 1413-1416.
576) Takeshi Oka, “Interstellar H3+,” Proceedings of the National Academy of Sciences, USA 103 (2006): 12235-12242.
