Planetary Magnetic Dynamo Effect on Atmospheric Protection of Early Earth and Mars

Déhant, V.; Lämmer, H.; Kulikov, Yu. N.; Grießmeier, J.-M.; Breuer, D.; Verhoeven, O.; Karatekin, Özgür; Hoolst, Tim Van; Korablev, Oleg; Lognonné, Philippe

doi:10.1007/978-0-387-74288-5_10

Cited by 12 publications

(7 citation statements)

References 120 publications

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“…The escape limit is typically characterized as being in either the diffusion or energy limited regime, with no connection to the presence of a magnetic field. However, it is commonly argued that magnetic field strength should play an important role in atmospheric escape [Michel, 1971;Chassefiere, 1997;Lundin et al, 2007;Dehant et al, 2007;Lammer et al, 2012;Owen and Adams, 2014;Brain et al, 2014]. Below we speculate about how a magnetic field could influence escape.…”

Section: Magnetic Limited Escapementioning

confidence: 90%

Whole planet coupling between climate, mantle, and core: Implications for rocky planet evolution

Foley

Driscoll

2016

Geochem Geophys Geosyst

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Earth's climate, mantle, and core interact over geologic timescales. Climate influences whether plate tectonics can take place on a planet, with cool climates being favorable for plate tectonics because they enhance stresses in the lithosphere, suppress plate boundary annealing, and promote hydration and weakening of the lithosphere. Plate tectonics plays a vital role in the long-term carbon cycle, which helps to maintain a temperate climate. Plate tectonics provides long-term cooling of the core, which is vital for generating a magnetic field, and the magnetic field is capable of shielding atmospheric volatiles from the solar wind. Coupling between climate, mantle, and core can potentially explain the divergent evolution of Earth and Venus. As Venus lies too close to the sun for liquid water to exist, there is no long-term carbon cycle and thus an extremely hot climate. Therefore plate tectonics cannot operate and a long-lived core dynamo cannot be sustained due to insufficient core cooling. On planets within the habitable zone where liquid water is possible, a wide range of evolutionary scenarios can take place depending on initial atmospheric composition, bulk volatile content, or the timing of when plate tectonics initiates, among other factors. Many of these evolutionary trajectories would render the planet uninhabitable. However, there is still significant uncertainty over the nature of the coupling between climate, mantle, and core. Future work is needed to constrain potential evolutionary scenarios and the likelihood of an Earth-like evolution.

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Section: Magnetic Limited Escapementioning

confidence: 90%

Whole planet coupling between climate, mantle, and core: Implications for rocky planet evolution

Foley

Driscoll

2016

Geochem Geophys Geosyst

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“…Due to the EUV heating and expansion of the upper atmosphere an early martian magnetic field could have not most likely protect the ion escape of C + and O + atoms which originated from dissociation of CO 2 molecules. By applying the same test-particle model, as in the study of early Earth by Lichtenegger et al (2010), to the upper atmosphere profiles and estimated martian magnetopause distances as given in Dehant et al (2007), we can show that the expanded thermosphere-exosphere can interact with the solar wind plasma which results in pick up C + ion escape fluxes of >10 11 cm s −1 before 4 Gyr ago. Thus, due to the high activity of young Sun and the low gravity of Mars a dense early Noachian martian atmosphere may not have built up during the first 300-400 Myr after the planet's origin.…”

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

confidence: 91%

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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“…One can see that the sputter loss was probably similar to that of ion erosion and for sure not efficient enough to cause the loss of that hundreds of mbar of CO 2 could be lost. Further, we note that the sputtering is a highly nonlinear process that depends on the EUV flux and the life time of the martian magnetic dynamo (Dehant et al 2007). Furthermore, it was shown by Terada et al (2009) that, due to the extreme solar wind atmosphere interaction caused by the young Sun before ∼4 Gyr ago, a stronger induced magnetic field in the upper atmosphere could have decreased sputtering during the transition period when the planet's intrinsic dynamo stopped working.…”

Section: Environmental Effects Of the Late Heavy Bombardmentmentioning

confidence: 91%

Outgassing History and Escape of the Martian Atmosphere and Water Inventory

et al. 2012

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The evolution and escape of the martian atmosphere and the planet's water inventory can be separated into an early and late evolutionary epoch. The first epoch started from the planet's origin and lasted ∼500 Myr. Because of the high EUV flux of the young Sun and Mars' low gravity it was accompanied by hydrodynamic blow-off of hydrogen and strong thermal escape rates of dragged heavier species such as O and C atoms. After the main part of the protoatmosphere was lost, impact-related volatiles and mantle outgassing may have resulted in accumulation of a secondary CO 2 atmosphere of a few tens to a few hundred mbar around ∼4-4.3 Gyr ago.

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Planetary Magnetic Dynamo Effect on Atmospheric Protection of Early Earth and Mars

Cited by 12 publications

References 120 publications

Whole planet coupling between climate, mantle, and core: Implications for rocky planet evolution

Whole planet coupling between climate, mantle, and core: Implications for rocky planet evolution

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

Outgassing History and Escape of the Martian Atmosphere and Water Inventory

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