Outgassing History and Escape of the Martian Atmosphere and Water Inventory

Lämmer, H.; Chassefière, Éric; Karatekin, Özgür; Morschhauser, A.; Niles, P. B.; Mousis, O.; Odert, P.; Möstl, U. V.; Breuer, D.; Déhant, V.; Grott, M.; Gröller, H.; Hauber, Ernst; Pham, Lê Binh San

doi:10.1007/s11214-012-9943-8

Cited by 164 publications

(145 citation statements)

References 214 publications

(282 reference statements)

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“…5 shows that the highest obtainable values of M tot are less than 1 × 10 20 kg. If we take the minimum disk model to estimate M tot 7 × 10 18 kg and use a mass fraction of 20% for water in a comet nucleus, guided by Rosetta results for comet 67P (Rotundi et al 2015), we obtain about 10 m Global Equivalent Layer, which is much less than the estimated total inventory of martian water (Lammer et al 2013). We conclude that the presence of liquid water on the surface of Mars during the Noachian did not occur because the planet swept up its water at that time through the LHB.…”

Section: The Largest Cometary Impactorsmentioning

confidence: 95%

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Cometary impact rates on the Moon and planets during the late heavy bombardment

Rickman

Wiśniowski

Gabryszewski

et al. 2017

A&A

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Context. The Nice model predicts that the trans-planetary planetesimal disk made a large or even dominant contribution to the cratering in the inner solar system during the late heavy bombardment (LHB). In the presence of evidence that lunar craters and mare basins may be mainly of asteroidal origin, there is a dilemma of the missing comets that is not yet resolved. Aims. We aim to revisit the problem of cometary impact rates on the Moon and the terrestrial planets during the LHB with a flexible model, allowing us to study the influences of physical destruction of comets, the mass of the primordial disk, and the distribution of this mass over the entire size range. Methods. We performed a Monte Carlo study of the dynamics of the cometary LHB projectiles and derive the impact rates by calculating individual collision probabilities for a huge sample of projectile orbits. We used Minimum Orbit Intersection Distances (MOIDs) according to a new scheme introduced here. Different calculations were performed using different models for the physical evolution of comet nuclei and for the properties of the primordial, trans-planetary disk. Results. Based on the capture probability of Jupiter Trojans, we find a best fit radius of the largest LHB comet impacting the Moon for a low-mass primordial disk. For this disk mass, the LHB cratering of the Moon, Mercury and Mars were dominated by asteroids. However, some smaller lunar maria were likely preceded by comet impacts. The volatile delivery to the Earth and Mars by LHB comets was much less than their water inventories. Conclusions. There is no excessive cometary cratering, if the LHB was caused by a late planetary instability in the Nice Model. The Earth and Mars obtained their water very early in their histories. The Noachian water flows on Mars cannot be attributed to the arrival of LHB-related H 2 O or CO 2 .

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Section: The Largest Cometary Impactorsmentioning

confidence: 95%

“…In addition, there is an open question about the amount of volatile delivery to Mars during the LHB (see Lammer et al 2013). In the current paper we aim to address these issues by a quantitative estimate of the timeintegrated lunar and planetary impact rates for a projectile population of the cometary type.…”

Section: Introductionmentioning

confidence: 99%

Cometary impact rates on the Moon and planets during the late heavy bombardment

Rickman

Wiśniowski

Gabryszewski

et al. 2017

A&A

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“…6 in Lammer et al 2013). On the other hand, values of m crit /m tan between 10−30 can remove some atmosphere, but not very efficiently, since even for the most favorable conditions, a 1 bar protoatmosphere could not have been eroded to present values over the age of the solar system (Shuvalov & Artemieva 2001;Ivanov 2001;Svetsov 2007;Pham et al 2009;Lammer et al 2013, and references therein). Thus, impact erosion seems to be a less efficient atmosphere escape process compared to hydrodynamic loss powered by the soft X-rays and extreme ultraviolet (XUV) radiation of the young active Sun, that was expected to be about 100 times higher compared to today's solar value (Ribas et al 2005;Claire et al 2012).…”

Section: Influence On Catastrophically Outgassed Steam Atmospheresmentioning

confidence: 99%

“…Ratios ≥30 accumulate atmosphere from several mbar up to more than 10 bar if m crit /m tan reaches a value of 2400 (see Fig. 6 in Lammer et al 2013). On the other hand, values of m crit /m tan between 10−30 can remove some atmosphere, but not very efficiently, since even for the most favorable conditions, a 1 bar protoatmosphere could not have been eroded to present values over the age of the solar system (Shuvalov & Artemieva 2001;Ivanov 2001;Svetsov 2007;Pham et al 2009;Lammer et al 2013, and references therein).…”

Section: Influence On Catastrophically Outgassed Steam Atmospheresmentioning

confidence: 99%

“…However, as mentioned before frequent impacts as modeled in this study will also evaporate lakes or most likely prevent the formation of large lakes or oceans during the XUV saturation phase of the young Sun. On the other hand, as discussed in Lammer et al (2013) impacts may also deliver additional volatiles that could be incorporated in the planetary environment after the XUV flux of the young Sun has decreased after the first few 100 Myr so that a secondary atmosphere could grow. However, the surface temperature enhancement by frequent impacts during the first 100 Myr should keep a catastrophically outgassed steam atmosphere at 1.5 AU in vapor form longer than 0.1 Myr, at least periodically.…”

Section: Influence On Catastrophically Outgassed Steam Atmospheresmentioning

confidence: 99%

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Impact induced surface heating by planetesimals on early Mars

Maindl¹,

Dvořák²,

Lämmer³

et al. 2015

A&A

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Aims. We investigate the influence of impacts of large planetesimals and small planetary embryos on the early Martian surface on the hydrodynamic escape of an early steam atmosphere that is exposed to the high soft X-ray and extreme-ultraviolet (EUV) flux of the young Sun. Methods. Impact statistics in terms of number, masses, velocities, and angles of asteroid impacts onto early Mars are determined via n-body integrations. Based on these statistics, smoothed particle hydrodynamics (SPH) simulations result in estimates of energy transfer into the planetary surface material and the resulting surface heating. For the estimation of the atmospheric escape rates we applied a soft X-ray and EUV absorption model and a 1D upper atmosphere hydrodynamic model to a magma ocean-related catastrophically outgassed steam atmosphere with surface pressure values of 52 bar H 2 O and 11 bar CO 2 . Results. The estimated impact rates and energy deposition onto an early Martian surface can account for substantial heating. The energy influx and conversion rate into internal energy is probably sufficient to keep a shallow magma ocean liquid for an extended period of time. Higher surface temperatures keep the outgassed steam atmosphere longer in vapor form and therefore enhance its escape to space within ∼0.6 Myr after its formation.

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Solar cycle effects on the ion escape from Mars

Lundin

Barabash

Holmström

et al. 2013

Geophysical Research Letters

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Solar cycle effects on the escape of planetary ions from Mars are investigated using Mars Express Analyzer of Space Plasmas and Energetic Atoms 3 data from June 2007 to January 2013. Average and median tail fluxes of low‐energy (<300 eV) heavy ions (O+, O2+), derived from the full data set covering 7900 orbits, are highly correlated with the solar activity proxies F10.7 and the sunspot number, Ri. The average heavy ion escape rate increased by a factor of ≈ 10, from ≈ 1 · 1024 s−1 (solar minimum) to ≈ 1 · 1025 s−1 (solar maximum). Combining data from this, and other studies, an empiric model/expression is derived for the Martian escape rate versus solar activity F10.7 and Ri. The model is a useful tool to derive the accumulated ion escape rate from Mars based on historical records of solar activity, with potentials back to the young Sun époque.

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Outgassing History and Escape of the Martian Atmosphere and Water Inventory

Cited by 164 publications

References 214 publications

Cometary impact rates on the Moon and planets during the late heavy bombardment

Cometary impact rates on the Moon and planets during the late heavy bombardment

Impact induced surface heating by planetesimals on early Mars

Solar cycle effects on the ion escape from Mars

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