Aeronomical evidence for higher CO2 levels during Earth’s Hadean epoch

Lichtenegger, Herbert; Lämmer, H.; Grießmeier, J.-M.; Kulikov, Yu. N.; Paris, Philip von; Hausleitner, W.; Krauß, Sandro; Rauer, H.

doi:10.1016/j.icarus.2010.06.042

Cited by 97 publications

(125 citation statements)

References 54 publications

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“…(4)- (6) and r = 1 AU yields a similar evolution of the mass loss rate as indicated by the shaded area in Fig. 1, valid for main-sequence G-type stars with an age of at least 0.7 Gyr Lichtenegger et al, 2010).…”

Section: The Time Evolution Of the Solar Windsupporting

confidence: 70%

“…These parameters for a Sun-like star can be estimated as a function of the age from the observations discussed above, together with an empirical model for an age-dependence of the solar/stellar wind velocity (Newkirk Jr., 1980;Grießmeier et al, 2004Grießmeier et al, , 2007Lichtenegger et al, 2010) …”

Section: The Time Evolution Of the Solar Windmentioning

confidence: 99%

“…In some cases the thermosphere may expand beyond an atmosphere protecting magnetospheric shield. Highly irradiated terrestrial planets can thus be even in danger of being stripped of their whole atmospheres Lammer et al, 2009;Lichtenegger et al, 2010).…”

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 99%

“…In the hydrodynamic flow regime, the major gases in the thermosphere can expand very efficiently to several planetary radii above the planetary surface. As a result light atoms experience high thermal escape rates and expand to large distances (Tian et al, 2008a where the whole atmosphere may be eroded by solar/stellar wind plasma flow related non-thermal escape processes Lammer et al, 2007;Lundin et al, 2007;Lichtenegger et al, 2010). 5.1 Hydrogen-rich upper atmospheres of terrestrial planets Terrestrial planets may evolve through phases where their upper atmospheres are hydrogen-rich.…”

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 99%

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Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

et al. 2012

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It is shown that the evolution of planetary atmospheres can only be understood if one recognizes the fact that the radiation and particle environment of the Sun or a planet's host star were not always on the same level as at present. New insights and the latest observations and research regarding the evolution of the solar radiation, plasma environment and solar/stellar magnetic field derived from the observations of solar proxies with different ages will be given. We show that the extreme radiation and plasma environments of the young Sun/stars have important implications for the evolution of planetary atmospheres and may be responsible for the fact that planets with low gravity like early Mars most likely never build up a dense atmosphere during the first few 100 Myr after their origin. Finally we present an innovative new idea on how hydrogen clouds and energetic neutral atom (ENA) observations around transiting Earth-like exoplanets by space observatories such as the WSO-UV, can be used for validating the addressed atmospheric evolution studies. Such observations would enhance our understanding on the impact on the activity of the young Sun on the early atmospheres of Venus, Earth, Mars and other Solar System bodies as well as exoplanets.

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Section: The Time Evolution Of the Solar Windsupporting

confidence: 70%

Section: The Time Evolution Of the Solar Windmentioning

confidence: 99%

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 99%

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 99%

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Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

et al. 2012

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“…Depending on stellar activity and the strength of the planet's magnetic field, coronal mass ejection from highly active young stars may also erode substantial quantities of heavy gases from planetary atmospheres (Khodachenko et al 2007;Lammer et al 2007;Lichtenegger et al 2010). The situation is likely to be most severe for lower mass planets around M-stars, which can lose large amounts of CO 2 and N 2 if their magnetic moments are weak.…”

Section: Evolution Of Atmospheric Compositionmentioning

confidence: 99%

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES

Wordsworth

Pierrehumbert

2013

ApJ

199

169

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Water photolysis and hydrogen loss from the upper atmospheres of terrestrial planets is of fundamental importance to climate evolution but remains poorly understood in general. Here we present a range of calculations we performed to study the dependence of water loss rates from terrestrial planets on a range of atmospheric and external parameters. We show that CO 2 can only cause significant water loss by increasing surface temperatures over a narrow range of conditions, with cooling of the middle and upper atmosphere acting as a bottleneck on escape in other circumstances. Around G-stars, efficient loss only occurs on planets with intermediate CO 2 atmospheric partial pressures (0.1-1 bar) that receive a net flux close to the critical runaway greenhouse limit. Because G-star total luminosity increases with time but X-ray and ultraviolet/ultravoilet luminosity decreases, this places strong limits on water loss for planets like Earth. In contrast, for a CO 2 -rich early Venus, diffusion limits on water loss are only important if clouds caused strong cooling, implying that scenarios where the planet never had surface liquid water are indeed plausible. Around M-stars, water loss is primarily a function of orbital distance, with planets that absorb less flux than ∼270 W m −2 (global mean) unlikely to lose more than one Earth ocean of H 2 O over their lifetimes unless they lose all their atmospheric N 2 /CO 2 early on. Because of the variability of H 2 O delivery during accretion, our results suggest that many "Earth-like" exoplanets in the habitable zone may have ocean-covered surfaces, stable CO 2 /H 2 O-rich atmospheres, and high mean surface temperatures.

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Escape and evolution of Mars's CO₂ atmosphere: Influence of suprathermal atoms

et al. 2017

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With a Monte Carlo model we investigate the escape of hot oxygen and carbon from the Martian atmosphere for four points in time in its history corresponding to 1, 3, 10, and 20 times the present solar EUV flux. We study and discuss different sources of hot oxygen and carbon atoms in the thermosphere and their changing importance with the EUV flux. The increase of the production rates due to higher densities resulting from the higher EUV flux competes against the expansion of the thermosphere and corresponding increase in collisions. We find that the escape due to photodissociation increases with increasing EUV level. However, for the escape via some other reactions, e.g., dissociative recombination of O2+, this is only true until the EUV level reaches 10 times the present EUV flux and then the rates start to decrease. Furthermore, our results show that Mars could not have had a dense atmosphere at the end of the Noachian epoch, since such an atmosphere would not have been able to escape until today. In the pre‐Noachian era, most of the magma ocean and volcanic activity‐related outgassed CO2 atmosphere could have been lost thermally until the Noachian epoch, when nonthermal loss processes such as suprathermal atom escape became dominant. Thus, early Mars could have been hot and wet during the pre‐Noachian era with surface CO2 pressures larger than 1 bar during the first 300 Myr after the planet's origin.

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Aeronomical evidence for higher CO2 levels during Earth’s Hadean epoch

Cited by 97 publications

References 54 publications

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES

Escape and evolution of Mars's CO₂ atmosphere: Influence of suprathermal atoms

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Aeronomical evidence for higher CO2 levels during Earth’s Hadean epoch

Cited by 97 publications

References 54 publications

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

Variability of solar/stellar activity and magnetic field and its influence on planetary atmosphere evolution

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES

Escape and evolution of Mars's CO2 atmosphere: Influence of suprathermal atoms

Contact Info

Product

Resources

About

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES

Escape and evolution of Mars's CO₂ atmosphere: Influence of suprathermal atoms