H<sub>2</sub>O<sub>2</sub>-induced Greenhouse Warming on Oxidized Early Mars

Itō, Yūichi; Hashimoto, George L.; Takahashi, Yoshiyuki O.; Ishiwatari, Masaki; Kuramoto, Kiyoshi

doi:10.3847/1538-4357/ab7db4

Cited by 9 publications

(8 citation statements)

References 56 publications

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“…APTY should give complete coverage at infrared wavelengths. Recently APTY was used to suggest the importance of H 2 O 2 as a greenhouse gas on oxidised Early Mars [238] .…”

Section: H 2 O 2 Paper XVmentioning

confidence: 99%

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Tennyson

Yurchenko

Al-Refaie

et al. 2020

Journal of Quantitative Spectroscopy and Radiative Transfer

200

161

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The ExoMol database ( www.exomol.com ) provides molecular data for spectroscopic studies of hot atmospheres. While the data are intended for studies of exoplanets and other astronomical bodies, the dataset is widely applicable. The basic form of the database is extensive line lists; these are supplemented with partition functions, state lifetimes, cooling functions, Landé g-factors, temperature-dependent cross sections, opacities, pressure broadening parameters, k -coefficients and dipoles. This paper presents the latest release of the database which has been expanded to consider 80 molecules and 190 isotopologues totaling over 700 billion transitions. While the spectroscopic data are concentrated at infrared and visible wavelengths, ultraviolet transitions are being increasingly considered in response to requests from observers. The core of the database comes from the ExoMol project which primarily uses theoretical methods, albeit usually fine-tuned to reproduce laboratory spectra, to generate very extensive line lists for studies of hot bodies. The data have recently been supplemented by line lists derived from direct laboratory observations, albeit usually with the use of ab initio transition intensities. A major push in the new release is towards accurate characterisation of transition frequencies for use in high resolution studies of exoplanets and other bodies.

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“…APTY should give complete coverage at infrared wavelengths. Recently APTY was used to suggest the importance of H 2 O 2 as a greenhouse gas on oxidised Early Mars [238] .…”

Section: H 2 O 2 Paper XVmentioning

confidence: 99%

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Tennyson

Yurchenko

Al-Refaie

et al. 2020

Journal of Quantitative Spectroscopy and Radiative Transfer

200

161

View full text Add to dashboard Cite

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“…Several other studies further investigated climate warming through CO2-H2 collisional heating (e.g., Hayworth et al, 2020) and how H2 could have been enriched in the atmosphere of Noachian Mars (e.g., Chassefière et al, 2016;Tosca et al, 2018;Haberle et al, 2019). Moreover, another recent study (Ito et al, 2020) found that within an oxidized environment H2O2 gas of only 1 ppm in a 3 bar CO2atmosphere on early Mars could have raised its temperature above freezing.…”

Section: Photochemical Stability and Atmospheric Collapsementioning

confidence: 99%

Did Mars Possess a Dense Atmosphere During the First $\sim400$ Million Years?

Scherf

Lämmer

2020

Space Sci Rev

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It is not yet entirely clear whether Mars began as a warm and wet planet that evolved towards the present-day cold and dry body or if it always was cold and dry with just some sporadic episodes of liquid water on its surface. An important clue into this question can be gained by studying the earliest evolution of the Martian atmosphere and whether it was dense and stable to maintain a warm and wet climate or tenuous and susceptible to strong atmospheric escape. In this review we therefore discuss relevant aspects for the evolution and stability of a potential early Martian atmosphere. This contains the EUV flux evolution of the young Sun, the formation timescale and volatile inventory of the planet including volcanic degassing, impact delivery and removal, the loss of the catastrophically outgassed steam atmosphere, atmosphere-surface interactions, as well as thermal and non-thermal escape processes affecting a potential secondary atmosphere at early Mars. While early non-thermal escape at Mars before 4 billion years ago is poorly understood, in particular in view of its ancient intrinsic magnetic field, research on thermal escape processes and the stability of a CO2-dominated atmosphere around Mars against high EUV fluxes indicate that volatile delivery and volcanic degassing cannot counterbalance the strong thermal escape. Therefore, a catastrophically

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“…The simulation with a high sursat ratio (Figure 7e) reaches slightly lower relative humidity in the upper layers compared to the arid simulation and still is not able to provide a significant warming, despite our ambition to model a more humid atmosphere in this scenario. As a consequence, we are not able to create a highly supersaturated layer in the upper atmosphere as is done in Ito et al (2020) with H 2 O 2 . The extreme case presented in Figure 7f is surprising in the fact that the surface temperature pattern is not similar to the other simulations.…”

Section: Idealized Wet Simulationmentioning

confidence: 98%

Water Supersaturation for Early Mars

et al. 2023

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Evidence of past liquid water flowing on the surface of Mars has been identified since the first orbital mission to the planet. However, reconstructing the climate that would allow liquid water at the surface is still an intense area of research. Previous studies showed that an atmosphere composed only of CO2 and H2O could not sustain surface temperatures above the freezing point of water. Different solutions have been studied, ranging from events like impacts on different atmospheric compositions, or even radiative feedback of water clouds that would create a dramatic greenhouse effect. In this context, we propose to study whether the supersaturation of water could warm the planet. Strong supersaturation is observed in the present‐day Martian atmosphere. On early Mars, supersaturation could enhance the greenhouse effect through strong absorption of the IR flux by water vapor or by modifying water clouds. While 1D modeling suggests a significant impact, our 3D model shows that warming the climate of early Mars requires a high supersaturation ratio, especially in the lower layers of the atmosphere. This configuration seems highly unrealistic since the level of supersaturation is higher than what would be expected in a dense atmosphere.

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H₂O₂-induced Greenhouse Warming on Oxidized Early Mars

Cited by 9 publications

References 56 publications

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Did Mars Possess a Dense Atmosphere During the First $\sim400$ Million Years?

Water Supersaturation for Early Mars

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H2O2-induced Greenhouse Warming on Oxidized Early Mars

Cited by 9 publications

References 56 publications

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres

Did Mars Possess a Dense Atmosphere During the First $\sim400$ Million Years?

Water Supersaturation for Early Mars

Contact Info

Product

Resources

About

H₂O₂-induced Greenhouse Warming on Oxidized Early Mars