Floral volatiles structure plant-pollinator interactions ...
Volatiles of Inner Solar System Bodies · Volatiles of Inner Solar System Bodies •Cosmochemistry...
Transcript of Volatiles of Inner Solar System Bodies · Volatiles of Inner Solar System Bodies •Cosmochemistry...
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Volatiles of Inner Solar System Bodies
James Greenwood
E&ES
& Planetary Sciences
Wesleyan University,
Connecticut USA Origin of Volatiles in Habitable Planets: The Solar System and Beyond
University of Michigan, October 16-17, 2017 James Greenwood, Wesleyan University
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Volatiles of Inner Solar System Bodies
• Cosmochemistry 101
• Volatiles of
– Mercury
– Venus
– Moon
– Mars
• New Model for origin of inner solar system hydrogen, oxygen, and nitrogen
James Greenwood, Wesleyan University
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1:1 correlation between Sun and CI chondrite James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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Cosmochemical fractionations
• The elements are fractionated in meteorites and planets based on these basic properties
– Physical and chemical processes lead to fractionations
– Gas-solid: Evaporation: condensation processes
– Also gas-liquid (evaporation-condensation)
– Physical fractionations (sorting by size)
– Oxidation/reduction
– Planetary differentiation
– Igneous fractionations (geochemical fractionations)
James Greenwood, Wesleyan University
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Elemental abundances in CR2 chondrites normalized to CI-no difference between siderophile, chalcophile,
or lithophile James Greenwood, Wesleyan University
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Carbonaceous Chondrites normalized to CI and Si
James Greenwood, Wesleyan University
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Carbonaceous Chondrites normalized to CI and Si
K
N C H
James Greenwood, Wesleyan University
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Ordinary and CV chondrites
James Greenwood, Wesleyan University
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Loss of volatiles during planetary formation
Refractory vs. Refractory for inner solar system
Volatile vs. Refractory for inner solar system
James Greenwood, Wesleyan University
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McCubbin
et al. (2012)
GRL
L09202,
doi:10.1029
/2012GL051711, 2012
James Greenwood, Wesleyan University
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Mercury- A volatile-rich planet
James Greenwood, Wesleyan University
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Cl vs. K Evans et al. (2015) Icarus 257, 417-427
James Greenwood, Wesleyan University
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Arecibo radar anomalies at
Mercury pole
James Greenwood, Wesleyan University
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Messenger at Mercury
Topographic lows
James Greenwood, Wesleyan University
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Lucey (2013) Science 339 282-283
James Greenwood, Wesleyan University
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Hollows on Mercury
James Greenwood, Wesleyan University
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Paige et al. (2013) Science 339, 300-303
James Greenwood, Wesleyan University
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Mercury-summary
• Mercury has high intrinsic levels of volatile elements (K, Cl, S)
• Cl-rich volcanic terrains • Graphite ‘anti-crust’ suggests no shortage of Carbon • Hollows point to recent volatile loss in craters • Mercury has water ice in permanently shadowed craters in
north polar region • The ice is apparently covered with an organic-rich lag
deposit that protects the water ice from sublimating away • Ice and organics may be cometary derived in recent times,
or…
James Greenwood, Wesleyan University
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Venus first look-Mariner 10
James Greenwood, Wesleyan University
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Venus topography
James Greenwood, Wesleyan University
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Venusian surface
James Greenwood, Wesleyan University
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Venus-summary
• Highly fractionated D/H (120 x Earth) suggests almost complete loss of water from the current atmosphere
• Venus likely received as many volatiles as Earth (why not?)
• C and N of Venus atmosphere similar to Earth abundances
• Means early Venus could have been similar to Early Earth in atmosphere and surface conditions (conducive to life too?)
• Venusian tesserae likely preserve evidence of previous volatile-rich weathering environment
James Greenwood, Wesleyan University
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Gilmore et al. (2017) Space Sci. Rev. DOI 10.1007/s11214-017-0370-8
James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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Moon
• Formed in giant impact with Mars-sized body
• Had giant magma ocean
• Youngest lavas ~ 1 Ga
• What happened to volatiles in this process?
James Greenwood, Wesleyan University
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Mars-sized impact into proto-Earth to form Moon-U.S. version
James Greenwood, Wesleyan University
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Moon’s volatile depletion
James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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Scenario 1: T = 2500K δ41K moon <= δ41K earth P ~10 bar Silicate atmosphere around magma disk Scenario 2: T = 3700K δ41K moon> δ41K earth P = 20bar
James Greenwood, Wesleyan University
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Lunar magmatic evolution
James Greenwood, Wesleyan University
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Vesiculated basalt from Apollo 15
James Greenwood, Wesleyan University
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Cameca ims 1270 SIMS Hokkaido University
James Greenwood, Wesleyan University
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1H SCAPS of 10044 apatite
James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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Moon -Summary
• Likely less water than Earth
• But still plenty of volatiles (?)
• High Cl and Zn isotope signatures likely due to magma ocean degassing
• Overall high D/H may be partial result of magma ocean degassing
• Low D/H of lunar samples likely solar wind contamination of near-surface magmas
James Greenwood, Wesleyan University
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Mars
James Greenwood, Wesleyan University
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Past oceans on Mars? James Greenwood, Wesleyan University
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What about Mars?
• Had early, aqueous environment near surface or at surface
• Conditions on Mars surface ~4.0-4.4 Ga may have been similar to Earth at this same time
• But how much water? Was there running water on the surface for millions of years, or just short wet episodes (thousands of years)
• Conditions on early Mars same as on early Earth – Early Earth saw the origin of life, why not Mars? – Did life come from Mars on a meteorite? Or did Earth
seed early Mars??
James Greenwood, Wesleyan University
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What the Curiosity Rover sees
James Greenwood, Wesleyan University
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Sedimentary layers at Mars
James Greenwood, Wesleyan University
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Martian hydrologic landforms
James Greenwood, Wesleyan University
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Mars Topography 65˚N-65˚S
James Greenwood, Wesleyan University
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Fig. 5. Sketch of the alteration history of Mars, with phyllosilicates formed first, then sulfates,
then anhydrous ferric oxides.
J Bibring et al. Science 2006;312:400-404
Published by AAAS
James Greenwood, Wesleyan University
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Villanueva et al. (2015) Science, 348 218-221
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Hydrodynamic Escape
• Elevated levels of heavy isotopes of hydrogen, nitrogen, carbon, oxygen, and noble gases
• Classic example of hydrodynamic escape due to early blow-off of hydrogen that carries all the other atmospheric gases away, which can cause mass-dependent isotope fractionation if the conditions are right (Hunten et al., 1987)
• If loss is at too high a rate, or the event is too rapid, the loss of the atmosphere does not lead to isotopic fractionation
James Greenwood, Wesleyan University
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Watson et al., (1994)
Science, 265 86-90
James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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2003
James Greenwood, Wesleyan University
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2015
James Greenwood, Wesleyan University
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2017
NWA 7034
Los Angeles
James Greenwood, Wesleyan University
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Shergotty
James Greenwood, Wesleyan University
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Hydrodynamic escape?
NWA 7034
Los Angeles
James Greenwood, Wesleyan University
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Then from 4.0 to 2.0 Ga a homogeneous, well-
mixed water reservoir, then atmospheric escape?
NWA 7034
Los Angeles
James Greenwood, Wesleyan University
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OR, early chondritic delivery of water, followed by
cometary delivery, leaving mantle and crustal reservoirs
unmixed, due to no plate tectonics on Mars
NWA 7034
Los Angeles
James Greenwood, Wesleyan University
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Intermediate D/H crustal reservoir is frozen and can only contribute
small amounts to atmosphere during obliquity cycles-is this the
intermediate reservoir of Usui et al. (2015), also sampled by NWA
7034 (McCubbin et al., Goldschmidt Yokohama)??
NWA 7034
Los Angeles
James Greenwood, Wesleyan University
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Villanueva et al. (2015) Science, 348 218-221
James Greenwood, Wesleyan University
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Kurokawa et al. (2014) EPSL 394 179-185 Water loss in two episodes to reflect the dichotomy at ALH
84001.
James Greenwood, Wesleyan University
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Kurokawa et al. (2014) EPSL 394 179-185.
James Greenwood, Wesleyan University
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Estimates of water on Mars for ALH 84001 dD=+1960‰
• After Kurokawa et al. 2014:
•𝑀𝑝
𝑀𝑐= (
𝐼𝑐
𝐼𝑝)11−𝑓
• Where Mp=GEL of past water reservoir (in
m), Mc is the current water inventory, Ic is the D/H of the current water inventory, and Ip the D/H of the past water inventory
James Greenwood, Wesleyan University
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Present water reservoir depends on the size of past reservoir, its D/H, and how it
was lost (fractionation factor, f)
• If Mc= 21 m (current water in the PLD), Ic: dD=+6412‰ (Los Angeles apatite), then we estimate Mp=54 m
• 54 m is much lower than estimates based on geology (Carr and Head (2003) estimate 130 m minimum GEL to 1500 m GEL)
• If Carr and Head are correct, then we are missing ~75 m of water, which could be buried ice (3x the current PLD?!)
• This estimate assumes no early loss of water due to hydrodynamic escape or early EUV induced loss of atmosphere (e.g. Lammer et al., 2013)
James Greenwood, Wesleyan University
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Present water reservoir depends on the size of past reservoir, its D/H, and how it
was lost (fractionation factor, f)
• If Mc= 21 m (current water in the PLD), Ic: dD=+6412‰ (Los Angeles apatite), then we estimate Mp=54 m
• 54 m is much lower than estimates based on geology (Carr and Head (2003) estimate 130 m minimum GEL to 1500 m GEL)
• If Carr and Head are correct, then we are missing ~75 m of water, which could be buried ice (3x the current PLD?!)
• This estimate assumes no early loss of water due to hydrodynamic escape or early EUV induced loss of atmosphere (e.g. Lammer et al., 2013)
63% loss of water James Greenwood, Wesleyan University
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Mars-what MAVEN sees
James Greenwood, Wesleyan University
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MAVEN-Mars Atmosphere Volatile EvolutioN Mission
James Greenwood, Wesleyan University
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At least 65% of the atmosphere has been lost to space over time
James Greenwood, Wesleyan University
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Mars Summary
• Still not sure of mantle volatile content and total abundance of Martian volatiles
• Mars could be best preserved example of cometary delivery of water and volatiles to inner solar system due to lack of plate tectonics.
• (WARNING: Highly controversial idea!)
James Greenwood, Wesleyan University
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Solar System D/H
Venus
James Greenwood, Wesleyan University
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Interplanetary Dust Particles (IDPs)
James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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D/H in the solar system
• Sun is D-depleted object (low D/H), and also similar to ISM (interstellar medium)
• Hotspots in IDP’s have very high D/H, similar to molecular clouds
• Everything else in solar system is in between these two endmembers
• Is it a mixing line between solar H and D-rich materials, like hotspots in IDP’s?
James Greenwood, Wesleyan University
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Sources of water for the inner solar system
• Extreme enriched D and 15N organic matter in chondrites similar to enrichment of these isotopes in interstellar molecules
• Nitrogen and Oxygen isotopes seem to require mixing of isotopically distinct sources
James Greenwood, Wesleyan University
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Furi and Marty (2015) Nat. Geosci.
James Greenwood, Wesleyan University
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Oxygen isotopes of the solar system
June 2011 James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University
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New model: Mixing of Outer Solar System Ices and Protosolar Gas
James Greenwood, Wesleyan University
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Water and Volatile Delivery to the Inner Solar System
• D/H can be simply explained as mixing of protosolar nebula hydrogen and outer solar system ice – Can also explain nitrogen and oxygen isotopes of inner
solar system materials
– Timing would suggest very early to explain the oxygen isotopes of planetary materials
• This model would suggest only minor additions of volatiles after initial accretion
• WARNING: Highly controversial new idea!
James Greenwood, Wesleyan University
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Questions?
Acknowledgements: This talk is based on work for the chapter “Delivery of water and volatiles to the inner solar system” for the ISSI Book “The delivery of water to proto-planets, planets, and satellites” Authors: James P. Greenwood, Shun Karato, Kathleen Vander Kaaden, Kaveh Pahlevan, and Tomohiro Usui James Greenwood, Wesleyan University
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James Greenwood, Wesleyan University