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VOL. 29, NO. 12 | DECEMBER 2019
The Faint Young Sun Problem Revisited SCIENCE EDITOR GSA is soliciting applications for three science co-editors for the journal Geology. The our ear terms begin anuar . Duties include: ensuring stringent peer OPENINGS review and expeditious processing of manuscripts; making nal acceptance or rejection decisions after considering reviewer recommendations; and, along with your co-editors, setting the editorial tone of Geology and maintaining excellent FOR content through publication of a diverse range of papers. Geology editors should expect to handle 200–250 manuscripts each year, with ~35 active manuscripts on any given day. 2021
3 POSITIONS AVAILABLE
GEOLOGY Research interests that complement those of the GEOLOGY continuing editors include, but are not limited to: geochemistry, geomorphology, petrology, tectonics, tectonophysics, structural geology, seismology, volcanology, Earth surface processes, planetary geology, Quaternary studies, hydrogeology, and economic geology.
Note: Because of the volume of papers received by Geology and the breadth of the topics covered, editors must be willing to handle papers outside of their main disciplines. A SUCCESSFUL EDITOR WILL HAVE: } a broad interest and experience in geosciences, TO APPLY including familiarity with new trends; Submit the following to Jeanette Hammann, hammann geoso iet org: } experience as an editor } A letter detailing how your experience (including editorial or associate editor for experience) quali es you for a science editor position, and a geoscience journal } A urri ulum vitae (experience with a GSA publication is preferred The GSA Publications Committee will review applications at its spring but not required); 2020 meeting. The Committee won’t consider incomplete applications. } international recognition and familiarity with many Editors work out of their current locations at work or at home. The geoscientists and their positions are considered voluntary, but GSA provides an annual stipend work; and funds for of ce expenses. First consideration will be given to nominations or applications received by ar h . } a progressive attitude and a willingness to take risks and encourage innovation; } ability to make timely decisions; and } a sense of perspective and humor.
GSA encourages applications from all quali ed persons and is committed to diversity. DECEMBER 2019 | VOLUME 29, NUMBER 12 SCIENCE 4 The Faint Young Sun Problem Revisited Jon Spencer GSA TODAY (ISSN 1052-5173 USPS 0456-530) prints news and information for more than 22,000 GSA member readers Cover: Composite of two images, one of the solar corona as seen and subscribing libraries, with 11 monthly issues (March- during the total solar eclipse of 21 Aug. 2017, the other of the solar disk April is a combined issue). GSA TODAY is published by The at ultraviolet frequencies as imaged by the Solar Dynamics Observa- ® Geological Society of America Inc. (GSA) with offices at tory satellite. Streamers from polar regions are areas where solar wind 3300 Penrose Place, Boulder, Colorado, USA, and a mail- ing address of P.O. Box 9140, Boulder, CO 80301-9140, USA. flows outward along magnetic field lines. At lower solar latitudes, GSA provides this and other forums for the presentation arcing magnetic-field lines are associated with sunspots and other surface activity that can yield of diverse opinions and positions by scientists worldwide, explosive coronal mass ejections. Both solar wind and mass ejections carry away mass and angular regardless of race, citizenship, gender, sexual orientation, momentum. This type of solar activity was much greater during the Sun’s fast-spinning youth. religion, or political viewpoint. Opinions presented in this publication do not reflect official positions of the Society. Image provided by Miloslav Druckmüller, Institute of Mathematics, Faculty of Mechanical Engineering, Brno University of Technology, Czech Republic. See related article, p. 4–10. © 2019 The Geological Society of America Inc. All rights reserved. Copyright not claimed on content prepared wholly by U.S. government employees within the scope of their employment. Individual scientists are hereby granted permission, without fees or request to GSA, to use a single 12 2020 Graduate Student Research Grants figure, table, and/or brief paragraph of text in subsequent work and to make/print unlimited copies of items in GSA TODAY for noncommercial use in classrooms to further 12 J. David Lowell Field Camp Scholarships education and science. In addition, an author has the right to use his or her article or a portion of the article in a thesis 12 Travel Awards to the 2020 Northeastern-Southeastern Joint Section Meeting or dissertation without requesting permission from GSA, provided the bibliographic citation and the GSA copyright credit line are given on the appropriate pages. For any 13 GSA GeoCorpsTM America Program other use, contact [email protected]. Subscriptions: GSA members: Contact GSA Sales & Service, 13 National Park Service Geoscientists-in-the-Parks (GIP) Opportunities +1-888-443-4472; +1-303-357-1000 option 3; gsaservice@ geosociety.org for information and/or to place a claim for non-receipt or damaged copies. Nonmembers and institutions: 14 Why GSA Membership Is Important to Me GSA TODAY is US$102/yr; to subscribe, or for claims for non-receipt and damaged copies, contact gsaservice@ 15 2020 Section Meetings Calendar geosociety.org. Claims are honored for one year; please allow sufficient delivery time for overseas copies. Peri- odicals postage paid at Boulder, Colorado, USA, and at 16 Preliminary Announcement and Call for Papers: GSA North-Central additional mailing offices. Postmaster: Send address Section Meeting changes to GSA Sales & Service, P.O. Box 9140, Boulder, CO 80301-9140. 20 Second Announcement: GSA South-Central Section Meeting GSA TODAY STAFF Executive Director and Publisher: Vicki S. McConnell 24 Second Announcement: Joint Meeting: Southeastern Section and Science Editors: Mihai N. Ducea, University of Arizona, Northeastern Section Dept. of Geosciences, Gould-Simpson Building, 1040 E 4th Street, Tucson, Arizona 85721, USA, [email protected] .edu; Peter Copeland, University of Houston, Department 30 Call for Applications: 2020–2021 GSA-USGS Congressional Science Fellow of Earth and Atmospheric Sciences, Science & Research Building 1, 3507 Cullen Blvd., Room 314, Houston, Texas 31 Geoscience Jobs & Opportunities 77204-5008, USA, [email protected]. Member Communications Manager: Matt Hudson, 37 GSA Foundation Update [email protected] Managing Editor: Kristen “Kea” Giles, [email protected], 39 Call for Proposals: GSA 2020 Annual Meeting & Exposition [email protected] Graphics Production: Emily Levine, [email protected] Advertising Manager: Ann Crawford, +1-800-472-1988 ext. 1053; +1-303-357-1053; Fax: +1-303-357-1070; [email protected] GSA Online: www.geosociety.org GSA TODAY: www.geosociety.org/gsatoday Printed in the USA using pure soy inks. The Faint Young Sun Problem Revisited
Jon Spencer, Dept. of Geosciences, University of Arizona, Tucson, Arizona 85721, USA, [email protected]
ABSTRACT INTRODUCTION known as the “faint young Sun problem” Earth and Mars should have been frozen The basic concepts involved in stellar- (Ulrich, 1975; Feulner, 2012). This article worlds in their early history because of energy generation were known by the is a brief review of solar evolution and the lower solar luminosity but were not, 1950s and include the insight that stellar faint young Sun problem for Earth and which challenges our understanding of luminosity gradually increases over time Mars that highlights recent developments. early atmospheres and surface conditions because of increasing density in stellar and/or our understanding of solar evolu- cores resulting directly from thermonu- STELLAR ENERGY PRODUCTION tion. This is known as the “faint young clear fusion (e.g., Burbidge et al., 1957) Stars form by gravitational contraction Sun problem.” One resolution to the (Fig. 1). Solar luminosity at birth was cal- of clouds of interstellar gas dominated by problem is that the Sun was more mas- culated to be ~70% of modern luminosity. hydrogen. During contraction and adia- sive and luminous in its youth before The idea that Earth should have geologic batic heating, increasing stellar energy blowing off mass. Astrophysical studies evidence of its presumably frozen youth production by nuclear fusion of hydrogen of stellar evolution and behavior, how- was gradually determined to be inconsis- into helium eventually terminates gravita- ever, including recent analysis of Kepler tent with growing evidence for liquid tional contraction (e.g., Haxton et al., space-telescope data, indicate that mass water at the surface of Archean Earth. 2013). Over millions of years, helium pro- loss is both insufficient and occurs too The problem was first addressed by duced by fusion of hydrogen accumulates early to allow for a more luminous Sun Sagan and Mullen (1972), who proposed in the cores of stars and increases core after ca. 4 Ga. Alternatively, greenhouse that atmospheric ammonia was crucial density, causing gravitational contraction gases were surprisingly effective at to early warming. More recent robotic and adiabatic heating which, in turn, raise warming young Earth and Mars. High exploration of Mars similarly indicates fusion rates and energy generation. This
concentrations of CO2 with the possible surprisingly warm and wet conditions process occurs gradually and continuously,
addition of biogenic CH4 are likely during its early geologic history. The dis- resulting in increasing core temperature dominant factors promoting open-water crepancy between low solar-energy pro- and total luminosity (Fig. 1) (Bahcall et al., conditions on Archean Earth. Evidence duction and warm early Earth and Mars is 2001). The Sun began with ~71% hydrogen of precipitation and flowing water on young Mars, including river valleys thousands of kilometers long, is more 1.4 problematic. Recent studies indicate that Gough (1981) (luminosity) 3–4 Ga river valleys and delta deposits surface temperature in crater lakes could have been produced 1.2 in <~107 years. Highly transient warm radius (r) periods during times of favorable orbital 1.0 parameters possibly led to brief melting
under otherwise icy conditions. Seasonal e 0.8 melting and runoff would be more likely 2 with ~1%–10% atmospheric H2 and CH4, area (r )
0.6 eenhous perhaps derived from serpentinization of luminosity olivine in the martian crust and released O gr from frozen ground by impacts and 0.4 2
volcanism, and/or derived directly from y H rt h volcanic outgassing. The recently recog- rt h 0.2 wa Ea nized effectiveness of hydrogen and Ea y (value relative to present value) runa on methane at absorbing infrared radiation on 0.0 in a thick CO2-dominated atmosphere, -4 -3 -2 -1 0123 in a process known as “collision-induced absorption,” is probably essential to the x (gigayears from present) solution to the faint young Sun problem Figure 1. Evolution of solar properties (from Bahcall et al., 2001). A simple approximation of solar- for Mars. luminosity evolution (Equation 1 of Gough, 1981) is also shown.
GSA Today, v. 29, https://doi.org/10.1130/GSATG403A.1. Copyright 2019, The Geological Society of America. CC-BY-NC.
4 GSA Today | December 2019 Figure 2. Known or hypothetical evolution of the 0.6 Sun, Earth, and Mars. (A) Star clusters, each containing stars of similar age, are plotted Stellar spindown A against rotation rate (Rebull et al., 2016, 2017; Pleiades th day) Meibom et al., 2009, 2011, 2015; Hartman et al., 0.4 2009). These are plotted as proxies for solar evolution, so cluster age on the horizontal axis M35 is plotted as distance from the left edge of the graph rather than the right edge. Curve show- 0.2 Praesepe ing approximate spindown rate is from Ayres t -0.6 (1997; t = time since cluster birth). (B) Ultraviolet M37 NGC 6811 NGC 6819 and X-ray radiation fluxes inferred for the Sun Sun
over time based on measured fluxes from (rotations per Ear nearby stars with approximate solar mass but 0.0 different ages (modified from Figure 8 of Ribas 30 et al., 2005). Current radiation flux = 1. (C) Evo- lution of solar luminosity for initial solar mass 0.1-2.0 nM (X-ray) Solar radiation B equal to, or slightly greater than, modern solar mass. The rate of mass loss is shown as pro- 20 portional to the rate of spindown of solar type 2-10 nM (soft X-ray and far ultraviolet) stars as shown in (A). Current luminosity = 1.0. Blue area at 3.2–3.5 Ga represents calculated 10-36 nM (ultraviolet) nM = nanometers (10-9 m) luminosity (~77%–79% of modern) at the time of 10 deposition of four stromatolite and microbial Radiation flux 92-120 nM (near ultraviolet) mat fossil units in northwest Australia and South Africa. (D) Some events in Earth history modern radiation flux = 1 that reflect climate and atmospheric composi- tion, including ages and names of Archean 0 stromatolite and microbial mat deposits older 1.0 than ca. 2.7 Ga and ages and names of glacial Solar luminosity deposits older than ca. 2.0 Ga. Archean glacial Mi = 1.04Mʘ deposits from Young et al. (1998; Mozaan), C Ojakangas et al. (2014; Talya), and de Wit and 0.9 Furnes (2016; Noisy) (cg—conglomerate). (E) Mi = 1.02Mʘ Some events in Mars history. Pre-Noachian magnetization of the martian crust ended Mi = 1.01Mʘ before formation of the Hellas impact basin. 0.8 Noachian to early Hesperian highland valley Solar luminosity networks formed after the large impact basins. Mi = initial solar mass
Mʘ = modern solar mass 0.7 Mi = 1.00Mʘ in its core and now has ~34%. The core will continue to contract, while the con- Hadean Archean Proterozoic Phanerozoic vecting outer layer will expand due to Archean stromatolites and microbial mats r e e oo l greater energy output from the core. Isu a D Dresse Mosher Earth Chobeni Moodies Belingw Buck Reef great oxidation event (GOE) Strelley P A BRIGHT YOUNG SUN? Mushandik Difficulties in identifying the causes of Noisy Complex, Onverwacht suite, Mozaan Group, S. Africa S. Africa warm climates on young Earth and Mars Talya cg, Dharwar craton, SW India glacial deposits >2 Ga provoked consideration of a more massive Huronian Supergroup, Ontario (brackets show uncertainty in age) Eastern Transvaal basin, S. Africa and therefore more luminous young Sun. Makganyene diamictite, S. Africa Specifically, if the Sun was 4%–5% more massive at its birth, before blowing off reducing atmosphere oxygenation of the atmosphere fractionation of sulfur isotopes fractionation of sulfur isotopes mass as solar wind and coronal mass ejec- independent of mass (MIF-S) dependent on mass tions, it could have provided elevated luminosity to warm the young planets to Noachian Hesperian Amazonian approximately modern temperatures (Fig. 2C) (Whitmire et al., 1995; Sackmann pre-Noachian and Boothroyd, 2003). This is plausible global magnetic eld (pre-Hellas) Mars E because stellar luminosity is very sensi- Hellas Isidis large impact basins (ages from Fassett and Head, 2011) tive to stellar mass. For a roughly solar- Argyre mass star, absolute luminosity scales to highland valley networks (ages from Fassett and Head, 2008a) almost the fifth power of solar mass, 4.0 3.0 2.0 1.0 0.0 while the greater gravitational attraction Age (Ga) of a more massive star reduces orbital radius proportional to mass. These factors together result in insolation at Earth and (1.01 raised to the 6.75 power ≈1.07; Minton stellar magnetic fields sweep through Mars that scales to almost the seventh and Malhotra, 2007). stellar winds and accelerate the winds power of solar mass such that a 1% The angular momentum of spinning circumferentially, thereby flinging the greater solar mass would result in ~7% stars is gradually carried away by stellar winds away and transferring angular greater insolation for orbiting planets winds. This is effective because rotating momentum from the star to the wind.
www.geosociety.org/gsatoday 5 Loss of angular momentum is more effec- rock units were deposited during open- al., 2018) and by sulfur isotopes in sedi- tive when stars spin faster, because mag- water, probably sunlit conditions (Figs. 2C mentary rocks that were fractionated inde- netic fields are generally stronger and and 2D). If Earth absorbed and retained pendent of mass by ultraviolet photolysis
sweep through stellar winds faster, and solar energy with modern effectiveness, of SO2 in an anoxic atmosphere (Farquhar because coronal mass ejections are more water at ancient Earth’s surface would and Wing, 2003; Claire et al., 2014;
common (e.g., Gallet and Bouvier, 2015). have been largely if not entirely frozen Dauphas and Schauble, 2016). CH4 and H2 Studies of star populations in clusters in during this time, except where heated by are potential greenhouse gases but would which all the stars have similar age indi- magmatic and hydrothermal activity or be slowly oxidized in such an atmosphere
cate that most stellar spindown, and by beneath hundreds to thousands of meters due to various reactions involving H2O and
inference mass loss, occurs during the first of ice. Geologic evidence of ancient warm CO2 that are triggered by ultraviolet radia- few hundred million years of a star’s life conditions is outlined below, followed by tion, a process that would be more effec- (Fig. 2A) (Skumanich, 1972; Ayres, 1997). possible explanations for effective surface tive with more intense short-wavelength This interpretation was strengthened by warming with a faint young Sun. radiation in the Archean (Pavlov et al., recent studies using data from the Kepler Archean strata deposited in shallow 2001; Catling and Kasting, 2017). Methane planet-finder satellite mission (active water with evidence of sunlit conditions could have been an important greenhouse 2009–2018). The Kepler telescope was indicate surface temperatures above gas, however, if methane-generating bacte- designed to detect changes in stellar lumi- freezing. These rock units include calcar- ria were abundant and if bacterial growth nosity resulting from passage of planets in eous and siliceous strata interpreted as was not inhibited by cooling due to sun- front of stars but also identified luminosity fossil microbial mats and mound-forming light-shielding organic haze produced by
variations due to transit of starspots on algal stromatolites that harbored, or were photochemical reactions involving CH4
stellar surfaces. This allowed determina- produced by, photosynthetic bacteria and CO2 (Domagal-Goldman et al., 2008). tion of rotation periods for thousands of (e.g., Grotzinger and Knoll, 1999; Noffke, Effective warming by reducing green- stars and accurate representation of stellar 2008; Tice et al., 2011). One of the oldest house gases is suggested by the coinci- spindown rates (Fig. 2A) (Meibom et al., examples of aquatic microbial life is the dence of earliest Proterozoic glaciations 2011, 2015; Rebull et al., 2017). It appears 3.42 Ga Buck Reef Chert in South Africa, with the great oxidation event (“GOE”) of from these studies that, if the Sun did have which contains carbonaceous layers, fila- Earth’s atmosphere (Holland, 2006) (Fig. greater mass during its youth, it would ments, and grains deposited within fine- 2D). The GOE would have destroyed
have lost most of that additional mass dur- grained, wave-agitated, siliceous sedi- atmospheric CH4 and H2, thereby causing ing rapid spindown before deposition of ments (Tice and Lowe, 2004) (Fig. 2D). the temperature drop (Pavlov et al., 2000; Archean algal stromatolites on Earth and The 3.35–3.43 Ga Strelley Pool Formation Haqq-Misra et al., 2008). Noachian river-channel incision and lake- in the Pilbara Supergroup of northwestern Three-dimensional climate models of delta deposition on Mars (Figs. 2C–2E). Australia (Wacey et al., 2010) contains Archean Earth’s atmosphere have been abundant evidence of microbial biofilms used to evaluate the effectiveness of sev- SOLAR RADIATION OVER TIME that precipitated carbonate and/or trapped eral atmospheric variables that are impor-
Short-wavelength solar radiation was fine detrital grains to form laminated tant for a warm climate, including CO2,
stronger during the Sun’s youth, which stromatolites (Allwood et al., 2009; CH4, and H2 concentration, absolute pres- further complicates warming scenarios Wacey, 2010; Duda et al., 2016). Multiple sure, and abundance of cloud-condensation because some greenhouse gases such as associated sedimentary features in the nuclei. Warm, open-water conditions not methane are readily photolyzed (broken Strelley Pool Formation, including rare unlike modern conditions were calculated
down) by such radiation or by free radicals desiccation cracks, indicate deposition in for a 1-bar atmosphere with 1% CO2 and
produced by photolysis of other gases shallow-water, tidally affected, marine 0.2% CH4 at 2.5 Ga (Charnay et al., 2013);
(Catling and Kasting, 2017). Six nearby environments (e.g., Allwood et al., 2006). 1.2% CO2 and 0.1% CH4 at 3.5 Ga (Le Hir
stars similar in mass to the Sun, but with a Fossil microbial mats and stromatolites et al., 2014); and 0.1–0.36 bar CO2 partial
range of ages, were identified by Ribas et resemble much younger and modern pressure with 1 bar N2 at 3.8 Ga (Charnay al. (2005) and used to estimate radiation microbial mats, photosynthetic stromato- et al., 2017). A variety of other factors characteristics of the Sun over time (Fig. lites, and cyanobacterial mounds influence global temperature, including 2B). Short-wavelength radiation, especially (Suosaari et al., 2016). sea-ice dynamics and the abundance far ultraviolet and X-ray, is significantly The abundance of sedimentary and of cloud-droplet condensation nuclei. more intense for younger stars because fossil indicators of liquid water at Earth’s Appropriate values of multiple variables their faster rotation rate increases the surface during the Archean indicates the appear to be capable of warming Archean accumulation of magnetic-field energy effectiveness of warming mechanisms that Earth to approximately modern tempera-
in stellar envelopes, which in turn results are still not well understood. CO2 and N2 tures, but the relative significance of these in greater short-wavelength radiation from were likely the dominant atmospheric factors in supporting warm conditions stellar surfaces and coronae. gases (Kasting, 2014; Catling and Kasting, under a faint young Sun has not been
2017). The absence of significant O2 in clearly identified. EARTH Earth’s Archean atmosphere is indicated Solar luminosity is calculated to have by unoxidized detrital sulfides and MARS been ~77%–79% of its current value at uraninite in Archean fluvial sediments The heavily cratered Noachian high- 3.2 –3.5 Ga, when at least four different (Rasmussen and Buick, 1999; Burron et lands of equatorial and southern Mars,
6 GSA Today | December 2019 which are the oldest exposed part of the Figure 3. (A) Obliquity of Mars at 2–6 Ma as cal- 50° martian crust, contain abundant evidence culated by Touma and Wisdom (1993). Note that obliquity exceeded 40° at 5–6 Ma. (B) Probability A of erosion by water. Mars is freezing cold of reaching high obliquities during the chaotic now and, with similar surface and atmo- obliquity evolution of Mars over a range of time 40° periods, with initial 25° obliquity (from Laskar et y spheric conditions, should have been even al., 2004). (C) Total annual insolation versus lati- colder at 3–4 Ga. Some drainages are tude for obliquity variation of 0°–90°. Insolation units are relative to the solar constant at 1.52 AU 30° thousands of kilometers long and were (from Ward, 1974). (D) Normalized density func- fed by numerous tributaries that reached tion for chaotic eccentricity variation for Mars Obliquit (from Figure 18d of Laskar et al., 2004). At pres- drainage divides in headwater regions ent eccentricity, solar insolation at perihelion 20° (Howard et al., 2005; Hynek et al., 2010). (orbital point closest to the Sun) is 45% greater Many rivers flowed into or through crater than at aphelion. lakes, and some left delta deposits (Irwin 10° 6 5 4 3 2 et al., 2005; Fassett and Head, 2008b; Age (Ma) Goudge et al., 2016). Calculations based obliquity is currently 23°, but because of on canyon width and depth indicate that stabilizing tidal forces associated with the 100 canyons reflect ~103–107 years of erosion Moon, obliquity varies over geologic time ) B and were not incised by catastrophic out- by <± 2° (Laskar et al., 1993). Mars, with 80 flows (Barnhart et al., 2009; Hoke et al., current obliquity of 25°, does not have a 2011; Rosenberg and Head, 2015). massive moon, and its obliquity is not 60 Precipitation, drainage incision, and similarly stabilized. Because of tidal crater-lake filling are inferred at ca. forces exerted on Mars by the Sun and 50 Ma 40 100 Ma 3.3–3.9 Ga based on crater density in planets, obliquity varied chaotically over 25 Ma 250 Ma affected terrains (Fassett and Head, millions of years to >60° (Figs. 3A and obability (percent Pr 20 10 Ma 2008a; Hoke and Hynek, 2009) (Fig. 2E). 3B) (Touma and Wisdom, 1993; Laskar 5 Ma Several factors would have supported et al., 2004). At obliquities >~45°, polar 0 warmer Noachian environmental condi- regions receive more sunlight than equa- 40° 50° 60° tions, although maybe not enough for pre- torial regions, potentially resulting in sea- Maximum obliquity (degrees) cipitation and flowing water. The pressure sonal sublimation and evaporation at high of the modern martian atmosphere, at 6–10 latitudes and snow at low latitudes at 0.5 millibars, is ~1% that of Earth, but the times near summer solstices (Fig. 3C) C ancient atmosphere was much thicker. The (Ward, 1974; Jakosky and Carr, 1985; 0.4 size and abundance of the smallest martian Wordsworth, 2016). High-latitude evapo- 75° 90° impact craters can be used to determine ration would be especially effective if the 0.3 60° atmospheric pressure because the smallest summer solstice coincided with greater 45° meteorites are slowed or destroyed during proximity to the Sun during a period of 0.2 passage through the atmosphere and so do high orbital eccentricity, which also 30° not create impact craters. Size-frequency varies chaotically (Fig. 3D). Annual insolation 0.1 15° distributions for craters in fluvial deposits Favorable obliquity and eccentricity, 0° near Gale crater indicate that Noachian and a thick CO2 atmosphere, may have 0.0 atmospheric pressure was in the range of been adequate for evaporation and subli- 90° 75° 60° 45° 30° 15° 0° ~1–2 bars during heavy Noachian bom- mation of ice at low elevations and accu- Latitude bardment (Kite et al., 2014). Atmospheric mulation of snow and ice at high eleva- pressure greater than a few hundred mil- tions, but warmer conditions are needed y D libars results in a vertical temperature pro- to melt snow and ice at high elevations 10 present file that approximates an adiabatic gradi- and produce runoff to carve river valleys ent (Wordsworth, 2016). Under such and fill lakes in the Noachian highlands 5 obabilit
conditions, surface temperatures are lower (Forget et al., 2012). Global climate mod- Pr 0 at higher elevation, with potential accumu- els indicate that 1%–10% hydrogen and 0.0 0.05 0.10 0.15 lation of snow and ice at high elevations. methane in a thick CO atmosphere could 2 Eccentricity Even if the atmosphere was pure CO2, have elevated temperatures sufficiently to however, this would not be adequate to melt ice at high elevations (Wordsworth warm early Mars to the point of supporting et al., 2017). These reduced gases are running water, especially in highland highly effective at absorbing infrared produce a weak bond in which the two regions (Kasting, 1991; Forget et al., 2012). radiation that would otherwise leave the gas molecules can absorb infrared radia- Orbital factors relevant to early Mars planet because of a process called “colli- tion that would not be absorbed by the climate are the variable tilt of its spin axis sion-induced absorption.” In this process, individual gas molecules. Collision- relative to the normal to the orbital plane extremely brief (~10–13 s) electrostatic induced absorption with these gases can (the obliquity) and the variable eccentric- interactions between colliding gas mol- potentially produce an early Mars atmo- ity (ellipticity) of the orbit. Earth’s ecules (CO2-H2 and CO2-CH4 in this case) sphere warm enough to cause melting and
www.geosociety.org/gsatoday 7 runoff from frozen martian highlands CONCLUSIONS Barnhart, C.J., Howard, A.D., and Moore, J.M., (Wordsworth et al., 2017). 1. Total solar-energy production is increas- 2009, Long-term precipitation and late- stage valley network formation: Landform Multispectral imaging, lander observa- ing gradually due to well-understood simulations of Parana Basin, Mars: Journal of tions, and the content of meteorites derived physics controlling rates of thermonu- Geophysical Research, v. 114, E01003, https:// from Mars indicate that olivine is common clear fusion in the solar core (Bahcall et doi.org/10.1029/2008JE003122. on Mars (e.g., McSween et al., 2006; al., 2001). A more massive and luminous Bradley, A., and Summons, R.E., 2010, Multiple Koeppen and Hamilton, 2008; Ody et al., young Sun is not supported by recent origins of methane at the Lost City Hydro- thermal Field: Earth and Planetary Science 2013). Hydrous alteration (serpentiniza- astrophysical studies. Letters, v. 297, p. 34–41, https://doi.org/ tion) of olivine and pyroxene by ground- 2. Archean sedimentary rocks on Earth 10.1016/j.epsl.2010.05.034. water should have been common if not include many indicators of liquid water Burbidge, E.M., Burbidge, G.R., Fowler, W.A., pervasive early in martian history (Oze at Earth’s surface, including sedimen- and Hoyle, F., 1957, Synthesis of the elements in stars: Reviews of Modern Physics, v. 29, and Sharma, 2005, 2007). Serpentinization tary rocks containing evidence of micro- no. 4, p. 547–650, https://doi.org/10.1103/ bial life that in turn indicate open water yields H2, which in turn reacts with CO2 to RevModPhys.29.547. with sunlight. The warm Archean Earth Burron, I., da Costa, G., Sharpe, R., Fayek, M., produce CH4, as is seen in hydrothermal fluids associated with ultramafic rocks resulted from high atmospheric concen- Gauert, C., and Hofmann, A., 2018, 3.2 Ga trations of CO , with possible additional detrital uraninite in the Witwatersrand Basin, on Earth (Bradley and Summons, 2010). 2 South Africa: Evidence of a reducing Archean Cooling of the young martian crust in the warming from methane and hydrogen, atmosphere: Geology, v. 46, p. 295–298, presence of groundwater would result in lower cloud albedo, a low ratio of land https://doi.org/10.1130/G39957.1. formation of a near-surface cryosphere of to water at Earth’s surface, and other Catling, D.C., and Kasting, J.F., 2017, Atmospheric frozen groundwater. Downward propaga- factors. It is not clear which additional Evolution on Inhabited and Lifeless Worlds: factors were dominant or if we are New York, Cambridge University Press, 579 p., tion of the boundary between frozen https://doi.org/10.1017/9781139020558. ground and deeper groundwater would missing something fundamental. Charnay, B., Forget, F., Wordsworth, R., Leconte, trap dissolved methane in methane clath- 3. Abundant evidence of martian river J., Millour, E., Codron, F., and Spiga, A., 2013, rate, which is water ice with ~6% methane channels and crater lakes at ca. 3.3–3.9 Exploring the faint young Sun problem and the Ga indicates warm conditions in other- possible climates of the Archean Earth with a trapped within the cage-like molecular 3-D GCM: Journal of Geophysical Research, structure of the clathrate ice (e.g., wise icy highlands of equatorial and v. 118, p. 10,414–10,431, doi:10.1002/jgrd.50808. Kvenvolden, 1993; Prieto-Ballesteros et southern Mars. Although transient Charnay, B., Le Hir, G., Fluteau, F., Forget, F., al., 2006). As a result of clathrate genesis, melting might occur under favorable and Catling, D.C., 2017, A warm or a cold the early martian cryosphere could have orbital parameters, augmentation of early Earth? New insights from a 3-D such warming by a few percent atmo- climate-carbon model: Earth and Planetary become a global methane reservoir (Lasue Science Letters, v. 474, p. 97–109, https:// et al., 2015). Furthermore, the cryosphere spheric H2 and CH4 released from doi.org/10.1016/j.epsl.2017.06.029. would become an impermeable cap for crustal or mantle reservoirs may be a Chassefière, E., Lasue, J., Langlais, B., and trapped gaseous H and CH , as on Earth viable solution to the faint young Sun Quesnel, Y., 2016, Early Mars serpentinization- 2 4 derived CH reservoirs, H -induced warming problem for Mars. 4 2 (Kvenvolden, 1993). and paleopressure evolution: Meteoritics & Methane and hydrogen liberated to the Planetary Science, v. 51, no. 11, p. 2234–2245, atmosphere by cryosphere disruption and ACKNOWLEDGMENTS https://doi.org/10.1111/maps.12784. melting from magmatism, impacts, and I thank James Kasting and an anonymous Claire, M.W., Kasting, J.F., Domagal-Goldman, reviewer for comments that improved clarity perhaps outburst floods, would result in S.D., Stüeken, E.E., Buick, R., and Meadows, and focus. V.S., 2014, Modeling the signature of sulfur minor to perhaps significant transient mass-independent fractionation produced in planetary warming. Such warming might the Archean atmosphere: Geochimica et have been sufficient to cause snow and REFERENCES CITED Cosmochimica Acta, v. 141, p. 365–380, Allwood, A.C., Walter, M.R., Kamber, B.S., ice melting and runoff from Noachian https://doi.org/10.1016/j.gca.2014.06.032. Marshall, C.P., and Burch, I.W., 2006, Dauphas, N., and Schauble, E.A., 2016, Mass highlands for perhaps tens to hundreds Stromatolite reef from the Early Archaean fractionation laws, mass-independent effects, of thousands of years (Chassefière et al., era of Australia: Nature, v. 441, p. 714–718, and isotopic anomalies: Annual Review of 2016; Wordsworth et al., 2017), especially https://doi.org/10.1038/nature04764. Earth and Planetary Sciences, v. 44, if it occurred during favorable orbital Allwood, A.C., Grotzinger, J.P., Knoll, A.H., p. 709–783, https://doi.org/10.1146/annurev Burch, I.W., Anderson, M.S., Coleman, M.L., parameters (Palumbo et al., 2018). Such -earth-060115-012157. and Kanik, I., 2009, Controls on development de Wit, M.J., and Furnes, H., 2016, 3.5-Ga warming could melt more methane and diversity of early Archean stromatolites: hydrothermal fields and diamictites in the clathrate in a positive feedback cycle Proceedings of the National Academy of Barberton Greenstone Belt—Paleoarchean (Wordsworth et al., 2017). Finally, the Sciences of the United States of America, crust in cold environments: Science Advances, 105–107 years needed for river valley inci- v. 106, no. 24, p. 9548–9555, https://doi.org/ v. 2, no. 2, e1500368, https://doi.org/10.1126/ 10.1073/pnas.0903323106. sciadv.1500368. sion was perhaps the cumulative result of Ayres, T.R., 1997, Evolution of the solar ionizing Domagal-Goldman, S.D., Kasting, J.F., Johnston, numerous short-lived warming episodes, flux: Journal of Geophysical Research, v. 102, E1, D.T., and Farquhar, J., 2008, Organic haze, each triggered by a different geologic p. 1641–1651, https://doi.org/10.1029/96JE03306. glaciations and multiple sulfur isotopes in event over hundreds of millions of years. Bahcall, J.N., Pinsonneault, M.H., and Basu, S., the Mid-Archean Era: Earth and Planetary 2001, Solar models: Current epoch and time Science Letters, v. 269, p. 29–40, https:// It remains uncertain, however, if all these dependences, neutrinos, and helioseismological doi.org/10.1016/j.epsl.2008.01.040. factors are adequate for melting and river- properties: The Astrophysical Journal, v. 555, Duda, J.-P., Van Kranendonk, M.J., Thiel, V., valley incision on Mars. p. 990–1012, https://doi.org/10.1086/321493. Ionescu, D., Strauss, H., Schäfer, N., and
8 GSA Today | December 2019 Reitner, J., 2016, A rare glimpse of Paleo- prospects: Annual Review of Astronomy and Laskar, J., Correia, A.C.M., Gastineau, M., archean life: Geobiology of an exceptionally Astrophysics, v. 51, p. 21–61, https://doi.org/ Joutel, F., Levrard, B., and Robutel, P., 2004, preserved microbial mat facies from the 10.1146/annurev-astro-081811-125539. Long term evolution and chaotic diffusion of 3.4 Ga Strelley Pool Formation, Western Hoke, M.R.T., and Hynek, B.M., 2009, Roaming the insolation quantities of Mars: Icarus, Australia: PLoS One, v. 11, no. 1, https:// zones of precipitation on ancient Mars as v. 170, p. 343–364, https://doi.org/10.1016/ doi.org/10.1371/journal.pone.0147629. recorded in valley networks: Journal of j.icarus.2004.04.005. Farquhar, J., and Wing, B.A., 2003, Multiple Geophysical Research, v. 114, E08002, Lasue, J., Quesnel, Y., Langlais, B., and Chasse- sulfur isotopes and the evolution of the https://doi.org/10.1029/2008JE003247. fière, E., 2015, Methane storage capacity of the atmosphere: Earth and Planetary Science Hoke, M.R.T., Hynek, B.M., and Tucker, G.E., early martian cryosphere: Icarus, v. 260, Letters, v. 213, p. 1–13, https://doi.org/ 2011, Formation timescales of large martian p. 205–214, https://doi.org/10.1016/j.icarus 10.1016/S0012-821X(03)00296-6. valley networks: Earth and Planetary Science .2015.07.010. Fassett, C.I., and Head, J.W., III, 2008a, The Letters, v. 312, p. 1–12, https://doi.org/10.1016/ Le Hir, G., Teitler, Y., Fluteau, F., Donnadieu, Y., and timing of martian valley network activity: j.epsl.2011.09.053. Philippot, P., 2014, The faint young Sun problem Constraints from buffered crater counting: Holland, H.D., 2006, The oxygenation of the revisited with a 3-D climate-carbon model— Icarus, v. 195, p. 61–89, https://doi.org/ atmosphere and oceans: Philosophical Part 1: Climate of the Past, v. 10, p. 697–713, 10.1016/j.icarus.2007.12.009. Transactions of the Royal Society of London, https://doi.org/10.5194/cp-10-697-2014. Fassett, C.I., and Head, J.W., III, 2008b, Valley Series B, Biological Sciences, v. 361, p. 903– McSween, H.Y., and 41 others, 2006, Character- network-fed, open-basin lakes on Mars: 915, https://doi.org/10.1098/rstb.2006.1838. ization and petrologic interpretation of Distribution and implications for Noachian Howard, A.D., Moore, J.M., and Irwin, R.P., III, olivine-rich basalts at Gusev Crater, Mars: surface and subsurface hydrology: Icarus, 2005, An intense terminal epoch of wide- Journal of Geophysical Research, v. 111, v. 198, p. 37–56, https://doi.org/10.1016/ spread fluvial activity on early Mars: 1. Valley E02S10, https://doi.org/10.1029/2005JE002477. j.icarus.2008.06.016. network incision and associated deposits: Meibom, S., Mathieu, R.D., and Stassun, K.G., Fassett, C.I., and Head, J.W., III, 2011, Sequence Journal of Geophysical Research, v. 110, 2009, Stellar rotation in M35: Mass-period and timing of conditions on early Mars: E12S14, https://doi.org/10.1029/2005JE002459. relations, spin-down rates, and gyrochronol- Icarus, v. 211, p. 1204–1214, https://doi.org/ Hynek, B.M., Beach, M., and Hoke, M.R.T., 2010, ogy: The Astrophysical Journal, v. 695, 10.1016/j.icarus.2010.11.014. Updated global map of martian valley networks p. 679–694, https://doi.org/10.1088/0004 Feulner, G., 2012, The faint young Sun problem: and implications for climate and hydrologic -637X/695/1/679. Reviews of Geophysics, v. 50, RG2006, processes: Journal of Geophysical Research, Meibom, S., and 19 others, 2011, The Kepler https://doi.org/10.1029/2011RG000375. v. 115, E09008, https://doi.org/10.1029/ cluster study: Stellar rotation in NGC 6811: Forget, F., Wordsworth, R., Millour, E., 2009JE003548. The Astrophysical Journal, Letters, v. 733, Madeleine, J.-B., Kerber, L., Leconte, J., Irwin, R.P., III, Howard, A.D., Craddock, R.A., https://doi.org/10.1088/2041-8205/733/1/L9. Marcq, E., and Haberle, R.M., 2012, 3D and Moore, J.M., 2005, An intense terminal Meibom, S., Barnes, S.A., Platais, I., Gilliland, modelling of the early martian climate under epoch of widespread fluvial activity on early R.L., Latham, D.W., and Mathieu, R.D., 2015,
a denser CO2 atmosphere: Temperatures and Mars: 2. Increased runoff and paleolake A spin-down clock for cool stars from
CO2 ice clouds: Icarus, v. 222, p. 81–99, development: Journal of Geophysical observations of a 2.5-billion-year-old cluster: https://doi.org/10.1016/j.icarus.2012.10.019. Research, v. 110, E12S15, https://doi.org/ Nature, v. 517, p. 589–591, https://doi.org/ Gallet, F., and Bouvier, J., 2015, Improved 10.1029/2005JE002460. 10.1038/nature14118. angular momentum evolution model for Jakosky, B.M., and Carr, M.H., 1985, Possible Minton, D.A., and Malhotra, R., 2007, Assessing solar-like stars II. Exploring the mass precipitation of ice at low latitudes of Mars the massive young Sun hypothesis to solve the dependence: Astronomy & Astrophysics, during periods of high obliquity: Nature, v. 315, warm young Earth puzzle: The Astrophysical v. 577, A98, https://doi.org/10.1051/0004-6361/ p. 559–561, https://doi.org/10.1038/315559a0. Journal, v. 660, p. 1700–1706, https://doi.org/
201525660. Kasting, J.F., 1991, CO2 condensation and the 10.1086/514331. Goudge, T.A., Fassett, C.I., Head, J.W., Mustard, climate of early Mars: Icarus, v. 94, p. 1–13, Noffke, N., 2008, Turbulent lifestyle: Microbial J.F., and Aureli, K.L., 2016, Insights into https://doi.org/10.1016/0019-1035(91)90137-I. mats on Earth’s sandy beaches—Today and surface runoff on early Mars from paleolake Kasting, J.F., 2014, Atmospheric composition of 3 billion years ago: GSA Today, v. 18, no. 10, basin morphology and stratigraphy: Geology, Hadean–early Archean Earth: The importance p. 4–9, https://doi.org/10.1130/GSATG7A.1. v. 44, no. 6, p. 419–422, https://doi.org/ of CO, in Shaw, G.H., ed., Earth’s Early Ody, A., Poulet, F., Bibring, J.-P., Loizeau, D., 10.1130/G37734.1. Atmosphere and Surface Environment: Carter, J., Gondet, B., and Langevin, Y., 2013, Gough, D.O., 1981, Solar interior structure and Geological Society of America Special Paper Global investigation of olivine on Mars: luminosity variations: Solar Physics, v. 74, 504, p. 19–28, https://doi.org/10.1130/ Insights into crust and mantle compositions: p. 21–34, https://doi.org/10.1007/BF00151270. 2014.2504(04). Journal of Geophysical Research, Planets, Grotzinger, J.P., and Knoll, A.H., 1999, Stromato- Kite, E.S., Williams, J.-P., Lucas, A., and v. 118, p. 234–262, https://doi.org/10.1029/ lites in Precambrian carbonates: Evolutionary Aharonson, O., 2014, Low palaeopressure of 2012JE004149. mileposts or environmental dipsticks?: Annual the martian atmosphere estimated from the Ojakangas, R.W., Srinivasan, R., Hegde, V.S., Review of Earth and Planetary Sciences, v. 27, size distribution of ancient craters: Nature Chandrakant, S.M., and Srikantia, S.V., 2014, p. 313–358, https://doi.org/10.1146/annurev Geoscience, v. 7, no. 5, p. 335–339, https:// The Talya Conglomerate: An Archean (~2.7 .earth.27.1.313. doi.org/10.1038/ngeo2137. Ga) glaciomarine formation, western Dharwar Haqq-Misra, J.D., Domagal-Goldman, S.D., Koeppen, W.C., and Hamilton, V.E., 2008, craton, southern India: Current Science, Kasting, P.J., and Kasting, J.F., 2008, A revised, Global distribution, composition, and v. 106, p. 387–396. hazy methane greenhouse for the Archean abundance of olivine on the surface of Mars Oze, C., and Sharma, M., 2005, Have olivine, Earth: Astrobiology, v. 8, no. 6, p. 1127–1137, from thermal infrared data: Journal of will gas: Serpentinization and the abiogenic https://doi.org/10.1089/ast.2007.0197. Geophysical Research, v. 113, E05001, production of methane on Mars: Geophysical Hartman, J.D., Gaudi, B.S., Pinsonneault, M.H., https://doi.org/10.1029/2007JE002984. Research Letters, v. 32, L10203, https:// Stanek, K.Z., Holman, M.J., McLeod, B.A., Kvenvolden, K.A., 1993, A primer on gas doi.org/10.1029/2005GL022691. Meibom, S., Barranco, J.A., and Kalirai, J.S., hydrates, in Howell, D.G., ed., The Future Oze, C., and Sharma, M., 2007, Serpentinization
2009, Deep MMT transit survey of the open of Energy Gases: U.S. Geological Survey and the inorganic synthesis of H2 in planetary cluster M37. III. Stellar rotation at 550 Myr: Professional Paper 1570, p. 279–291. surfaces: Icarus, v. 186, p. 557–561, https:// The Astrophysical Journal, v. 691, p. 342–364, Laskar, J., Joutel, F., and Robutel, P., 1993, doi.org/10.1016/j.icarus.2006.09.012. https://doi.org/10.1088/0004-637X/691/1/342. Stabilization of the Earth’s obliquity by the Palumbo, A.M., Head, J.W., and Wordsworth, Haxton, W.C., Robertson, R.G.H., and Serenelli, Moon: Nature, v. 361, p. 615–617, https:// R.D., 2018, Late Noachian Icy Highlands A.M., 2013, Solar neutrinos: Status and doi.org/10.1038/361615a0. climate model: Exploring the possibility of
www.geosociety.org/gsatoday 9 transient melting and fluvial/lacustrine Rosenberg, E.N., and Head, J.W., III, 2015, Late Wacey, D., 2010, Stromatolites in the ~3400 Ma activity through peak annual and seasonal Noachian fluvial erosion on Mars: Cumulative Strelley Pool Formation, Western Australia: temperatures: Icarus, v. 300, p. 261–286, water volumes required to carve the valley Examining biogenicity from the macro- to https://doi.org/10.1016/j.icarus.2017.09.007. networks and grain size of bed-sediment: the nano-scale: Astrobiology, v. 10, no. 4, Pavlov, A.A., Kasting, J.F., Brown, L.L., Rages, Planetary and Space Science, v. 117, p. 429–435, p. 381–395, https://doi.org/10.1089/ast.2009.0423. K.A., and Freedman, R., 2000, Greenhouse https://doi.org/10.1016/j.pss.2015.08.015. Wacey, D., McLoughlin, N., Stoakes, C.A., warming by CH in the atmosphere of early Sackmann, I.-J., and Boothroyd, A.I., 2003, Our 4 Kilburn, M.R., Green, O.R., and Brasier, Earth: Journal of Geophysical Research, Sun. V. A bright young Sun consistent with M.D., 2010, The 3426–3350 Ma Strelley Pool v. 105, E5, p. 11,981–11,990, https://doi.org/ helioseismology and warm temperatures on Formation in the East Strelley greenstone 10.1029/1999JE001134. ancient Earth and Mars: The Astrophysical belt—A field and petrographic guide: Pavlov, A.A., Brown, L.L., and Kasting, J.F., Journal, v. 583, p. 1024–1039, https://doi.org/ Geological Survey of Western Australia, 2001, UV shielding of NH3 and O2 by organic 10.1086/345408. hazes in the Archean atmosphere: Journal of Sagan, C., and Mullen, G., 1972, Earth and Mars: Record 2010/10, 64 p. Geophysical Research, v. 106, E10, p. 23,267– Evolution of atmospheres and surface Ward, W.R., 1974, Climatic variation on Mars 1. 23,287, https://doi.org/10.1029/2000JE001448. temperatures: Science, v. 177, p. 52–56, Astronomical theory of insolation: Journal of Prieto-Ballesteros, O., Kargel, J.S., Fairén, A.G., https://doi.org/10.1126/science.177.4043.52. Geophysical Research, v. 79, no. 24, p. 3375– Fernández-Remolar, D.C., Dohm, J.M., and Skumanich, A., 1972, Time scales for Ca II 3386, https://doi.org/10.1029/JC079i024p03375. Amils, R., 2006, Interglacial clathrate emission decay, rotational braking, and lithium Whitmire, D.P., Doyle, L.R., Reynolds, R.T., and destabilization on Mars: Possible contributing depletion: The Astrophysical Journal, v. 171, Matese, J.J., 1995, A slightly more massive source of its atmospheric methane: Geology, p. 565–567, https://doi.org/10.1086/151310. young Sun as an explanation for warm v. 34, no. 3, p. 149–152, https://doi.org/10.1130/ Suosaari, E.P., Reid, R.P., Playford, P.E., Foster, temperatures on early Mars: Journal of G22311.1. J.S., Stoltz, J., Casaburi, G., Hagan, P., Geophysical Research, v. 100, E3, p. 5457– Rasmussen, B., and Buick, R., 1999, Redox state of Chirayath, V., Macintyre, I., Planavsky, N., and 5464, https://doi.org/10.1029/94JE03080. the Archean atmosphere: Evidence from detrital Eberli, G.P., 2016, New multi-scale perspectives Wordsworth, R.D., 2016, The climate of early heavy minerals in ca. 3250–2750 Ma sandstones on the stromatolites of Shark Bay, Western Mars: Annual Review of Earth and Planetary from the Pilbara craton, Australia: Geology, Australia: Scientific Reports, v. 6, p. 20,557, Sciences, v. 44, p. 381–408, https://doi.org/ v. 27, p. 115–118, https://doi.org/10.1130/ https://doi.org/10.1038/srep20557. 0091-7613(1999)027<0115:RSOTAA>2.3.CO;2. Tice, M.M., and Lowe, D.R., 2004, Photosyn- 10.1146/annurev-earth-060115-012355. Rebull, L.M., and 18 others, 2016, Rotation in the thetic microbial mats in the 3,416-Myr-old Wordsworth, R., Kalugina, Y., Lokshtanov, S., Pleiades with K2. I. Data and first results: The ocean: Nature, v. 431, p. 549–552, https:// Vigasin, A., Ehlmann, B., Head, J., Sanders, C., Astronomical Journal, v. 152, https://doi.org/ doi.org/10.1038/nature02888. and Wang, H., 2017, Transient reducing 10.3847/0004-6256/152/5/113. Tice, M.M., Thornton, D.C.O., Pope, M.C., greenhouse warming on early Mars: Geophysi- Rebull, L.M., Stauffer, J.R., Hillenbrand, L.A., Olszewski, T.D., and Gong, J., 2011, Archean cal Research Letters, v. 44, p. 665–671, Cody, A.M., Bouvier, J., Soderblom, D.R., microbial mat communities: Annual Review https://doi.org/10.1002/2016GL071766. Pinsonneault, M., and Hebb, L., 2017, Rotation of Earth and Planetary Sciences, v. 39, Young, G.M., von Brunn, V., Gold, D.J.C., and of late-type stars in Praesepe with K2: The p. 297–319, https://doi.org/10.1146/annurev Minter, W.E.L., 1998, Earth’s oldest reported Astrophysical Journal, v. 829, https://doi.org/ -earth-040809-152356. glaciation: Physical and chemical evidence 10.3847/1538-4357/aa6aa4. Touma, J., and Wisdom, J., 1993, The chaotic from the Archean Mozaan Group (~2.9 Ga) of Ribas, I., Guinan, E.F., Güdel, M., and Audard, obliquity of Mars: Science, v. 259, p. 1294–1297, South Africa: The Journal of Geology, v. 106, M., 2005, Evolution of the solar activity over https://doi.org/10.1126/science.259.5099.1294. p. 523–538, https://doi.org/10.1086/516039. time and effects on planetary atmospheres. I. Ulrich, R.K., 1975, Solar neutrinos and variations High-energy irradiances (1–1700 Å): The in the solar luminosity: Science, v. 190, Manuscript received 24 Feb. 2019 Astrophysical Journal, v. 622, p. 680–694, p. 619–624, https://doi.org/10.1126/science Revised manuscript received 30 Apr. 2019 https://doi.org/10.1086/427977. .190.4215.619. Manuscript accepted 13 June 2019
10 GSA Today | December 2019 Geologist's Wish List
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THE GEOSCIENCE HANDBOOK 2016 AGI Data Sheets, Fifth Edition Compiled by Mark B. Carpenter Christopher M. Keane Graphics by Kat Cantner
v. 4.0
PICKS (Ma) AGE GEOLOGICAL SOCIETY OFMESOZOIC AMERICA 66.0 GEOLOGIC TIME SCALEEPOCH MAGNETIC 72.1 POLARITY PERIOD
AGE MAASTRICHTIAN
CHRON. ANOM. (Ma) HIST PICKS C30 30 83.6 (Ma) 31 C31 CAMPANIAN 86.3 AGE C32 0.01 70 32 89.8 CENOZOIC SANTONIAN 1.8 33 LATE EPOCH 2.6 C33 CONIACIAN 93.9 MAGNETIC CALABRIAN 3.6 . PERIOD TURONIAN POLARITY GELASIAN 80
HOLOCENE . * 100
AGE 5.3 N
CHRO PIACENZIAN
. NOM A ST (Ma) HI QUATER- PLEISTOCENE CENOMANIAN 1 C1 NARY ZANCLEAN 7.2 90 2 C2 PLIOCENE MESSINIAN ALBIAN 113 2A C2A C34 34 PALEOZOIC C3 3 100 AGE 11.6 5 TORTONIAN (Ma) PERIOD 3A C3A APTIAN 126 13.8 EPOCH 4 C4 110 31 4A C4A SERRAVALLIAN 1 AGE 16.0 EARLY 134 5 C5 BARREMIAN PICKS PRECAMBRIAN 10 LANGHIAN 260 Lopin- (Ma)
120 HAUTERIVIAN 39 AGE
M0r 1 CHANGHSINGIAN CRETACEOUS gian 5A C5A M1 (Ma) VALANGINIAN WUCHIAPINGIAN EON M3 Guada-145
20.4 M5 252 MIOCENE BURDIGALIAN C5B CAPITANIAN ERA 5B 130 BERRIASIAN280 lupian 254 15 M10
5C C5C 152 WORDIAN 260 NEOGENE 23.0 PERIOD 5D C5D M12 ROADIAN M14 TITHONIAN 265 BDY. C5E AQUITANIAN PERMIAN Cisura- 5E M16 157 KUNGURIAN C6 269 AGES 6 140 M18 lian 750 300 272 (Ma) C6A M20 KIMMERIDGIAN 164 ARTINSKIAN EDIACARAN 20 6A LATE 279 NEOPRO- M22 166 C6B CHATTIAN SAKMARIAN 541 6B 28.1 OXFORDIAN 168 TEROZOIC C6C 150 M25 LATE ASSELIAN 6C CALLOVIAN 170 290 CRYOGENIAN GZHELIAN 1000 635 7 C7 M29 320 BATHONIANMIDDLE 74 C7A 1KASIMOVIAN 296 7A VANIAN BAJOCIANPENNSYL- 299 8 C8 MOSCOVIAN 25 160 MIDDLE AALENIANEARLY 304 C9 TONIAN 9 RUPELIAN 307 850 33.9 BASHKIRIAN83 C10 LATE 1 1250 10 340 TOARCIAN 11 SERPUKHOVIAN 315
11 C OLIGOCENE 170 STENIAN CHANGES MIDDLE 191 MESOPRO- 1000 30 12 MISSIS- 323 C12 SIPPIAN 37.8 PLIENSBACHIAN TEROZOIC PRIABONIAN CARBONIFEROUS VISEAN 331 1500 180 360 EARLY EARLY 199 ECTASIAN 13 C13 1200
SINEMURIAN 201 C15 JURASSIC TOURNAISIAN 15 41.2 C16 35 16 BARTONIAN HETTANGIAN 347
C17 190 209 RAPID POLARITY RAPID 17 CHANGES POLARITY RAPID CALYMMIAN 380 LATE RHAETIANFAMENNIAN 359 1750 1400
18 C18 19 LUTETIAN 200 40 C19 FRASNIAN STATHERIAN 47.8 MIDDLE 372 1600 400 NORIAN 2000 20 DEVONIAN GIVETIAN C20 LATE EIFELIAN 228 PROTEROZOIC 210 383 PALEOPRO-
EOCENE 388 OROSIRIAN 1800 45 EARLY EMSIAN TEROZOIC 420 393 21 237 2250 C21 220 PRAGIANCARNIAN YPRESIAN 241
PRIDOLI LOCHKOVIAN PALEOGENE 408 22 C22 LUDLOW LADINIAN RHYACIAN 2050 56.0 411 247 WENLOCK LUDFORDIAN 50 C23 440230 ANISIAN 250 23 MIDDLEGORSTIAN 419 2525002 LLANDO- HOMERIAN 423
SILURIAN SHEINWOODIAN 24 59.2 VERY TRIASSIC OLENEKIAN426 THANETIAN TELYCHIAN INDUAN427 C24 SIDERIAN 2300 240 EARLYAERONIAN 430 61.6 460 RHUDDANIAN 433 LATE HIRNANTIAN 2750 NEOARCHEAN 55 SELANDIAN 439 25 C25 KATIAN 441 444 250 SANDBIAN 445 2500 26 MIDDLE C26 DANIAN 66.0480 DARRIWILIAN 453 60 458 3000 EARLY DAPINGIAN
27 C27 ORDOVICIAN PALEOCENE FLOIAN 467 MESO- C28 28 FURON- TREMADOCIAN 470 ARCHEAN 2800 29 500 C29 GIAN AGE 1 478 3250 65 JIANGSHANIAN0 30 C30 485 Epoch 3 PAIBIAN GUZHANGIAN 490 520 DRUMIAN 494 Epoch 2 AGE 5 497 PALEO- 501 3500 AGE 4 ARCHEAN 505 3200 CAMBRIAN AGE 3 509 ARCHEAN TERRE- 540 514 Get full-size chart: NEUVIANwww.gsapubs.orgAGE 2 521 3750 FORTUNIAN 529 EOARCHEAN 4000 3600 541 HADEAN FIELD TOOLS 3300 Penrose Place • P.O. Box 9140 • Boulder, CO 80301 4000 1-888-443-4472 • 1 © 2015
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