The Diversity of Planetary Atmospheric ChemistryLessons and Challenges from Our Solar System and Extrasolar Planets

被引:0
作者
Franklin P. Mills
Julianne I. Moses
Peter Gao
Shang-Min Tsai
机构
[1] Australian National University,Fenner School of Environment & Society
[2] Space Science Institute,McDonald Observatory
[3] University of Texas Austin,undefined
[4] University of California Berkeley,undefined
[5] University of Oxford,undefined
[6] University of Bern,undefined
来源
Space Science Reviews | 2021年 / 217卷
关键词
Atmospheric chemistry; Chemical modeling; Terrestrial planets; Giant planets; Titan; Exoplanets;
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摘要
Atmospheres in our solar system range from oxidizing to reducing, transient to dense, veiled by clouds and hazes to transparent. Observations already suggest that exoplanets exhibit an even more diverse range of atmospheric chemistry and composition. Nevertheless, there are commonalities across the atmospheres of our solar system that provide valuable guidance and lessons for observing and interpreting exoplanetary atmospheres. Lessons gleaned from decades of study of planetary atmospheric chemistry are synthesized and explored to understand their implications for exoplanets.
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[1]  
Agúndez M.(2014)Pseudo 2D chemical model of hot-Jupiter atmospheres: application to HD 209458b and HD 189733b Astron. Astrophys. 564 2881-2898
[2]  
Parmentier V.(2019)Advanced methods for uncertainty assessment and global sensitivity analysis of an Eulerian atmospheric chemistry transport model Atmos. Chem. Phys. 19 222-224
[3]  
Venot O.(1984)Cloud structure on the dark side of Venus Nature 307 65-71
[4]  
Hersant F.(2011)Clouds and chemistry in the atmosphere of extrasolar planet HR8799b Astrophys. J. 733 58-3776
[5]  
Selsis F.(2020)Vplanet: the virtual planet simulator Publ. Astron. Soc. Pac. 132 3759-573
[6]  
Aleksankina K.(2017)Night side distribution of SO Icarus 294 545-37
[7]  
Reis S.(2012) content in Venus’ upper mesosphere J. Geophys. Res. 117 19-184
[8]  
Vieno M.(2020)First detection of O J. Geophys. Res., Planets 125 157-L32
[9]  
Heal M.R.(1994) 1.27 μm nightglow emission at Mars with OMEGA/MEX and comparison with general circulation model predictions J. Geophys. Res. 99 L29-1063
[10]  
Allen D.A.(1988)Chemical cycling in the Venusian atmosphere: a full photochemical model from the surface to 110 km Icarus 73 1048-4593