Creation and Evolution of Impact-generated Reduced Atmospheres of Early Earth

  title={Creation and Evolution of Impact-generated Reduced Atmospheres of Early Earth},
  author={Kevin J. Zahnle and Roxana E. Lupu and David C. Catling and Nicholas Wogan},
  journal={arXiv: Earth and Planetary Astrophysics},
  • K. Zahnle, R. Lupu, +1 author N. Wogan
  • Published 31 December 2019
  • Physics, Environmental Science
  • arXiv: Earth and Planetary Astrophysics
The origin of life on Earth seems to demand a highly reduced early atmosphere, rich in CH4, H2, and NH3, but geological evidence suggests that Earth's mantle has always been relatively oxidized and its emissions dominated by CO2 H2O, and N2. The paradox can be resolved by exploiting the reducing power inherent in the "late veneer," i.e., material accreted by Earth after the Moon-forming impact. Isotopic evidence indicates that the late veneer consisted of extremely dry, highly reduced inner… 
Growth and evolution of secondary volcanic atmospheres: I. Identifying the geological character of warm rocky planets
The geology of Earth and super-Earth sized planets will, in many cases, only be observable via their atmospheres. Here, we use the creation of volcanic atmospheres as a key window into planetary
Hydrodynamic escape of an impact-generated reduced proto-atmosphere on Earth
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Redox state of Earth’s magma ocean and its Venus-like early atmosphere
Oxidation state of iron in Earth’s magma ocean indicates it would have produced a Venus-like early atmosphere upon cooling, which would have led to a prebiotic terrestrial atmosphere composed of CO2-N2, in proportions and at pressures akin to those observed on Venus.
Low volcanic outgassing rates for a stagnant lid Archean Earth with graphite-saturated magmas
Volcanic gases supplied a large part of Earth's early atmosphere, but constraints on their flux are scarce. Here we model how C-O-H outgassing could have evolved through the late Hadean and early
Evolution of the Earth’s atmosphere during Late Veneer accretion
Recent advances in our understanding of the dynamical history of the Solar system have altered the inferred bombardment history of the Earth during accretion of the Late Veneer, after the
Delayed and variable late Archaean atmospheric oxidation due to high collision rates on Earth
Frequent violent collisions of impactors from space punctuated the geological and atmospheric evolution of early Earth. It is generally accepted that the most massive collisions altered the chemistry
Vertically Resolved Magma Ocean–Protoatmosphere Evolution: H2, H2O, CO2, CH4, CO, O2, and N2 as Primary Absorbers
A coupled numerical framework is presented that links an evolutionary, vertically resolved model of the planetary silicate mantle with a radiative‐convective models of the atmosphere and investigates the early evolution of idealized Earth‐sized rocky planets with end‐member, clear‐sky atmospheres dominated by either H2, H2O, CO2, CH4, CO, O2, or N2.
Plausible Emergence and Self Assembly of a Primitive Phospholipid from Reduced Phosphorus on the Primordial Earth.
  • M. Gaylor, P. Miró, +14 authors Vytis Karanauskus
  • Medicine
    Origins of life and evolution of the biosphere : the journal of the International Society for the Study of the Origin of Life
  • 2021
It is hypothesized that a reduced phospholipid arises from Fischer-Tropsch-type (FTT) production of a C8 alkanoic acid, which condenses with an organophosphinate (derived from schreibersite corrosion to hypophosphite with subsequent methylation/oxidation), to yield a reduced protophospholipids.
Was Venus Ever Habitable? Constraints from a Coupled Interior–Atmosphere–Redox Evolution Model
Venus’s past climate evolution is uncertain. General circulation model simulations permit a habitable climate as late as ∼0.7 Ga, and there is suggestive—albeit inconclusive—evidence for previous
Oxygen controls on magmatism in rocky exoplanets
Experimental evidence is provided for a significant effect of planetary oxygen abundance on melting of rocks, showing that higher rock oxygen abundance leads to easier rock melting, implying that refractory oxygen abundance can directly control exoplanetary differentiation dynamics by affecting the conditions under which magmatism occurs, even in the absence of iron or volatiles.


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  • Geology, Medicine
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Planetary atmospheres depend fundamentally upon their geochemical inventory, temperature and the ability of their gravitational field to retain gases. In the case of Earth and other inner planets,
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High atmospheric CO/CO2 ratios are possible if either: the climate was cool (like today's climate), so that hydration of dissolved CO to formate was slow, or the formate formed from CO was efficiently converted into volatile, reduced carbon compounds, such as methane.
Massive impact-induced release of carbon and sulfur gases in the early Earth's atmosphere
Abstract Recent revisions to our understanding of the collisional history of the Hadean and early-Archean Earth indicate that large collisions may have been an important geophysical process. In this
Hydrogen-Nitrogen Greenhouse Warming in Earth's Early Atmosphere
It is shown that with an atmospheric composition consistent with the most recent constraints, the early Earth would have been significantly warmed by H2-N2 collision–induced absorption, key to warming the atmosphere of theEarly Earth.
Evolution of an Impact-Generated H2O–CO2 Atmosphere and Formation of a Hot Proto-Ocean on Earth
Abstract Due to impact degassing during accretion, a hot H2O-rich proto-atmosphere was possibly formed on the growing Earth. We investigate the evolution of an impact-generated H2O–CO2 atmosphere at
The chemical composition of the early terrestrial atmosphere: Formation of a reducing atmosphere from CI‐like material
[1] The chemical composition of Earth's early atmosphere is likely to have played an important role in the origin of life. In particular, the redox state of Earth's early atmosphere may have
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It is found that Fe2+ in a deep magma ocean would disproportionate to Fe3+ plus metallic iron at high pressures, which explains Earth’s carbon-rich interior and suggests that redox evolution during accretion was an important variable in determining the composition of the terrestrial atmosphere.
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If the atmosphere was reducing at any time during the last approximately 3900 Ma, high-temperature volcanic outgassing was not the cause of it and the results discussed in this article independently support the conclusion of Canil (1997, 1999).
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