Atmospheric and water loss from early Venus

Kulikov, Yu. N.; Lämmer, H.; Lichtenegger, Herbert; Terada, Naoki; Ribas, I.; Kolb, C.; Langmayr, D.; Lundin, R.; Guinan, E. F.; Barabash, S.; Biernat, H. K.

doi:10.1016/j.pss.2006.04.021

Cited by 132 publications

(174 citation statements)

References 119 publications

Supporting

Mentioning

162

Contrasting

Order By: Relevance

“…In recent studies by Kulikov et al (2006Kulikov et al ( , 2007, Lammer et al (2006Lammer et al ( , 2008, Lundin et al (2007), Tian et al (2008a, b) and illustrated in Fig. 4 it was shown that enhanced solar EUV radiation and plasma (winds, CMEs) should result in permanent forcing of the upper planetary atmospheres, which can ionize, heat, expand, chemically modify, and erode it during the early phase of a planetary lifetime.…”

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 96%

“…This behavior indicates that higher EUV fluxes during the young Sun periods should have also resulted in denser hot O coronae around Venus and Mars, resulting in higher pick up loss rates. Kulikov et al (2006) studied the expected O + ion pick up loss rates over Venus' history by using EUV data from solar proxies discussed in Section 2 and a range of solar wind plasma densities and velocities which were expected for the young active Sun. These authors used a diffusivegravitational equilibrium and thermal balance model, which was applied for a study of the heating of the early thermosphere by photodissociation and ionization processes, exothermic chemical reactions, and cooling by CO 2 IR emission in the 15 μm band.…”

Section: Response Of N 2 -Rich Atmospheres To High Euv Fluxesmentioning

confidence: 99%

“…The increase in solar luminosity over time and its climatological effect on Venus, Earth and Mars have been discussed by various authors in the past (e.g., Sagan and Mullen, 1972;Walker, 1975;Newman and Rood, 1977;Owen, 1979;Chassefière, 1996;Guinan and Ribas, 2002;Lammer et al, 2003;Ribas et al, 2005;Tian et al, 2005;Kulikov et al, 2006Kulikov et al, , 2007Cnossen et al, 2007). The early Sun, with a luminosity of about ∼70% of that today, should have been too faint to prevent the early Earth and Mars from freezing.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

et al. 2012

View full text Add to dashboard Cite

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.

show abstract

Section: Solar Activity Response Of Planetary Upper Atmospheresmentioning

confidence: 96%

Section: Response Of N 2 -Rich Atmospheres To High Euv Fluxesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

et al. 2012

View full text Add to dashboard Cite

show abstract

“…Pepin 1991), atmospheric loss because of escape to space (e.g. Kulikov et al 2007;Kulikov et al 2006) or incorporation into planetary surface material. But these processes are not known for the Gl 581 system.…”

Section: Model Input For Gl 581 and Performed Runsmentioning

confidence: 99%

The extrasolar planet Gliese 581d: a potentially habitable planet?

Paris

Gebauer

Godolt

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. The planetary system around the M star Gliese 581 contains at least three close-in potentially low-mass planets, Gl 581c, d, and e. In order to address the question of the habitability of Gl 581d, we performed detailed atmospheric modeling studies for several planetary scenarios. Methods. A 1D radiative-convective model was used to calculate temperature and pressure profiles of model atmospheres, which we assumed to be composed of molecular nitrogen, water, and carbon dioxide. The model allows for changing surface pressures caused by evaporation/condensation of water and carbon dioxide. Furthermore, the treatment of the energy transport has been improved in the model to account in particular for high CO 2 , high-pressure Super-Earth conditions. Results. For four high-pressure scenarios of our study, the resulting surface temperatures were above 273 K, indicating a potential habitability of the planet. These scenarios include three CO 2 -dominated atmospheres (95% CO 2 concentration with 5, 10, and 20 bar surface pressure) and a high-pressure CO 2 -enriched atmosphere (5% CO 2 concentration with 20 bar surface pressure). For all other considered scenarios, the calculated Gl 581d surface temperatures were below the freezing point of water, suggesting that Gl 581d would not be habitable then. The results for our CO 2 -dominated scenarios confirm very recent model results by Wordsworth et al. (2010). However, our model calculations imply that also atmospheres that are not CO 2 -dominated (i.e., 5% vmr instead of 95% vmr) could result in habitable conditions for Gl 581d.

show abstract

“…However, the strength of its 15 and 4.3 μm bands allows efficient cooling to space even at low pressures, so it also plays a key role in determining the cold-trap temperature (Pierrehumbert 2010). Finally, CO 2 can also directly limit the escape of hydrogen in the highest part of the atmosphere, because its effectiveness as an emitter of thermal radiation in the IR means it can "scavenge" energy that would otherwise be used to power hydrogen escape (Kulikov et al 2006;Tian et al 2009). The history of water on terrestrial planets should therefore be intimately related to that of carbon dioxide.…”

Section: Introductionmentioning

confidence: 99%

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES

Wordsworth

Pierrehumbert

2013

ApJ

188

169

View full text Add to dashboard Cite

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.

show abstract

Atmospheric and water loss from early Venus

Cited by 132 publications

References 119 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

The extrasolar planet Gliese 581d: a potentially habitable planet?

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES

Contact Info

Product

Resources

About

Atmospheric and water loss from early Venus

Cited by 132 publications

References 119 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

The extrasolar planet Gliese 581d: a potentially habitable planet?

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES

Contact Info

Product

Resources

About

WATER LOSS FROM TERRESTRIAL PLANETS WITH CO₂-RICH ATMOSPHERES