The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges

Cedric Gillmann; M. J. Way; Guillaume Avice; Doris Breuer; Gregor J. Golabek; Dennis Höning; Joshua Krissansen-Totton; Helmut Lammer; Joseph G. O’Rourke; Moa Persson; Ana Catalina Plesa; Arnaud Salvador; Manuel Scherf; Mikhail Y. Zolotov

doi:10.1007/s11214-022-00924-0

The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges

Cedric Gillmann, M. J. Way, Guillaume Avice, Doris Breuer^*, Gregor J. Golabek, Dennis Höning, Joshua Krissansen-Totton, Helmut Lammer, Joseph G. O’Rourke, Moa Persson, Ana Catalina Plesa, Arnaud Salvador, Manuel Scherf, Mikhail Y. Zolotov

^*Corresponding author for this work

Earth Sciences

Research output: Contribution to Journal › Review article › Academic › peer-review

Abstract

This work reviews the long-term evolution of the atmosphere of Venus, and modulation of its composition by interior/exterior cycling. The formation and evolution of Venus’s atmosphere, leading to contemporary surface conditions, remain hotly debated topics, and involve questions that tie into many disciplines. We explore these various inter-related mechanisms which shaped the evolution of the atmosphere, starting with the volatile sources and sinks. Going from the deep interior to the top of the atmosphere, we describe volcanic outgassing, surface-atmosphere interactions, and atmosphere escape. Furthermore, we address more complex aspects of the history of Venus, including the role of Late Accretion impacts, how magnetic field generation is tied into long-term evolution, and the implications of geochemical and geodynamical feedback cycles for atmospheric evolution. We highlight plausible end-member evolutionary pathways that Venus could have followed, from accretion to its present-day state, based on modeling and observations. In a first scenario, the planet was desiccated by atmospheric escape during the magma ocean phase. In a second scenario, Venus could have harbored surface liquid water for long periods of time, until its temperate climate was destabilized and it entered a runaway greenhouse phase. In a third scenario, Venus’s inefficient outgassing could have kept water inside the planet, where hydrogen was trapped in the core and the mantle was oxidized. We discuss existing evidence and future observations/missions required to refine our understanding of the planet’s history and of the complex feedback cycles between the interior, surface, and atmosphere that have been operating in the past, present or future of Venus.

Original language	English
Article number	56
Pages (from-to)	1-71
Number of pages	71
Journal	Space Science Reviews
Volume	218
Issue number	7
Early online date	7 Oct 2022
DOIs	https://doi.org/10.1007/s11214-022-00924-0
Publication status	Published - Oct 2022

Bibliographical note

Funding Information:
The authors thank S. Mojzsis and J. Head for their comments, as well as R. Wordsworth and an anonymous reviewer for their help in improving the manuscript. CG acknowledges the support of Rice University and the CLEVER planets group (itself supported by NASA and part of NExSS) and ET-HoME Excellence of Science programme. GA acknowledges support from the french Centre National d’Etudes Spatiales (CNES) for support of Venus-related studies. MJW acknowledges support from the Goddard Space Flight Center Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model. MJW acknowledges support from NASA’s Nexus for Exoplanet System Science (NExSS), the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model (ISFM) and the ROCKE-3D Project ISFM jointly funded by a NASA Planetary and Earth Science Divisions. AS acknowledges support from NASA’s Habitable Worlds Program (No. 80NSSC20K0226). MYZ acknowledges support from the NASA Solar System Workings program.

Publisher Copyright:
© 2022, The Author(s).

Funding

The authors thank S. Mojzsis and J. Head for their comments, as well as R. Wordsworth and an anonymous reviewer for their help in improving the manuscript. CG acknowledges the support of Rice University and the CLEVER planets group (itself supported by NASA and part of NExSS) and ET-HoME Excellence of Science programme. GA acknowledges support from the french Centre National d’Etudes Spatiales (CNES) for support of Venus-related studies. MJW acknowledges support from the Goddard Space Flight Center Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model. MJW acknowledges support from NASA’s Nexus for Exoplanet System Science (NExSS), the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model (ISFM) and the ROCKE-3D Project ISFM jointly funded by a NASA Planetary and Earth Science Divisions. AS acknowledges support from NASA’s Habitable Worlds Program (No. 80NSSC20K0226). MYZ acknowledges support from the NASA Solar System Workings program.

Keywords

Atmosphere
Coupled evolution
Feedback cycles
Venus
Volatile exchanges

UN SDGs

This output contributes to the following UN Sustainable Development Goals (SDGs)

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10.1007/s11214-022-00924-0

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Gillmann, C., Way, M. J., Avice, G., Breuer, D., Golabek, G. J., Höning, D., Krissansen-Totton, J., Lammer, H., O’Rourke, J. G., Persson, M., Plesa, A. C., Salvador, A., Scherf, M., & Zolotov, M. Y. (2022). The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges. Space Science Reviews, 218(7), 1-71. Article 56. https://doi.org/10.1007/s11214-022-00924-0

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title = "The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges",

abstract = "This work reviews the long-term evolution of the atmosphere of Venus, and modulation of its composition by interior/exterior cycling. The formation and evolution of Venus{\textquoteright}s atmosphere, leading to contemporary surface conditions, remain hotly debated topics, and involve questions that tie into many disciplines. We explore these various inter-related mechanisms which shaped the evolution of the atmosphere, starting with the volatile sources and sinks. Going from the deep interior to the top of the atmosphere, we describe volcanic outgassing, surface-atmosphere interactions, and atmosphere escape. Furthermore, we address more complex aspects of the history of Venus, including the role of Late Accretion impacts, how magnetic field generation is tied into long-term evolution, and the implications of geochemical and geodynamical feedback cycles for atmospheric evolution. We highlight plausible end-member evolutionary pathways that Venus could have followed, from accretion to its present-day state, based on modeling and observations. In a first scenario, the planet was desiccated by atmospheric escape during the magma ocean phase. In a second scenario, Venus could have harbored surface liquid water for long periods of time, until its temperate climate was destabilized and it entered a runaway greenhouse phase. In a third scenario, Venus{\textquoteright}s inefficient outgassing could have kept water inside the planet, where hydrogen was trapped in the core and the mantle was oxidized. We discuss existing evidence and future observations/missions required to refine our understanding of the planet{\textquoteright}s history and of the complex feedback cycles between the interior, surface, and atmosphere that have been operating in the past, present or future of Venus.",

keywords = "Atmosphere, Coupled evolution, Feedback cycles, Venus, Volatile exchanges",

author = "Cedric Gillmann and Way, \{M. J.\} and Guillaume Avice and Doris Breuer and Golabek, \{Gregor J.\} and Dennis H{\"o}ning and Joshua Krissansen-Totton and Helmut Lammer and O{\textquoteright}Rourke, \{Joseph G.\} and Moa Persson and Plesa, \{Ana Catalina\} and Arnaud Salvador and Manuel Scherf and Zolotov, \{Mikhail Y.\}",

note = "Funding Information: The authors thank S. Mojzsis and J. Head for their comments, as well as R. Wordsworth and an anonymous reviewer for their help in improving the manuscript. CG acknowledges the support of Rice University and the CLEVER planets group (itself supported by NASA and part of NExSS) and ET-HoME Excellence of Science programme. GA acknowledges support from the french Centre National d{\textquoteright}Etudes Spatiales (CNES) for support of Venus-related studies. MJW acknowledges support from the Goddard Space Flight Center Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division{\textquoteright}s Internal Scientist Funding Model. MJW acknowledges support from NASA{\textquoteright}s Nexus for Exoplanet System Science (NExSS), the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division{\textquoteright}s Internal Scientist Funding Model (ISFM) and the ROCKE-3D Project ISFM jointly funded by a NASA Planetary and Earth Science Divisions. AS acknowledges support from NASA{\textquoteright}s Habitable Worlds Program (No. 80NSSC20K0226). MYZ acknowledges support from the NASA Solar System Workings program. Publisher Copyright: {\textcopyright} 2022, The Author(s).",

year = "2022",

month = oct,

doi = "10.1007/s11214-022-00924-0",

language = "English",

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Gillmann, C, Way, MJ, Avice, G, Breuer, D, Golabek, GJ, Höning, D, Krissansen-Totton, J, Lammer, H, O’Rourke, JG, Persson, M, Plesa, AC, Salvador, A, Scherf, M & Zolotov, MY 2022, 'The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges', Space Science Reviews, vol. 218, no. 7, 56, pp. 1-71. https://doi.org/10.1007/s11214-022-00924-0

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AU - Avice, Guillaume

AU - Breuer, Doris

AU - Golabek, Gregor J.

AU - Höning, Dennis

AU - Krissansen-Totton, Joshua

AU - Lammer, Helmut

AU - O’Rourke, Joseph G.

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AU - Plesa, Ana Catalina

AU - Salvador, Arnaud

AU - Scherf, Manuel

AU - Zolotov, Mikhail Y.

N1 - Funding Information: The authors thank S. Mojzsis and J. Head for their comments, as well as R. Wordsworth and an anonymous reviewer for their help in improving the manuscript. CG acknowledges the support of Rice University and the CLEVER planets group (itself supported by NASA and part of NExSS) and ET-HoME Excellence of Science programme. GA acknowledges support from the french Centre National d’Etudes Spatiales (CNES) for support of Venus-related studies. MJW acknowledges support from the Goddard Space Flight Center Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model. MJW acknowledges support from NASA’s Nexus for Exoplanet System Science (NExSS), the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded by the NASA Planetary Science Division’s Internal Scientist Funding Model (ISFM) and the ROCKE-3D Project ISFM jointly funded by a NASA Planetary and Earth Science Divisions. AS acknowledges support from NASA’s Habitable Worlds Program (No. 80NSSC20K0226). MYZ acknowledges support from the NASA Solar System Workings program. Publisher Copyright: © 2022, The Author(s).

PY - 2022/10

Y1 - 2022/10

N2 - This work reviews the long-term evolution of the atmosphere of Venus, and modulation of its composition by interior/exterior cycling. The formation and evolution of Venus’s atmosphere, leading to contemporary surface conditions, remain hotly debated topics, and involve questions that tie into many disciplines. We explore these various inter-related mechanisms which shaped the evolution of the atmosphere, starting with the volatile sources and sinks. Going from the deep interior to the top of the atmosphere, we describe volcanic outgassing, surface-atmosphere interactions, and atmosphere escape. Furthermore, we address more complex aspects of the history of Venus, including the role of Late Accretion impacts, how magnetic field generation is tied into long-term evolution, and the implications of geochemical and geodynamical feedback cycles for atmospheric evolution. We highlight plausible end-member evolutionary pathways that Venus could have followed, from accretion to its present-day state, based on modeling and observations. In a first scenario, the planet was desiccated by atmospheric escape during the magma ocean phase. In a second scenario, Venus could have harbored surface liquid water for long periods of time, until its temperate climate was destabilized and it entered a runaway greenhouse phase. In a third scenario, Venus’s inefficient outgassing could have kept water inside the planet, where hydrogen was trapped in the core and the mantle was oxidized. We discuss existing evidence and future observations/missions required to refine our understanding of the planet’s history and of the complex feedback cycles between the interior, surface, and atmosphere that have been operating in the past, present or future of Venus.

AB - This work reviews the long-term evolution of the atmosphere of Venus, and modulation of its composition by interior/exterior cycling. The formation and evolution of Venus’s atmosphere, leading to contemporary surface conditions, remain hotly debated topics, and involve questions that tie into many disciplines. We explore these various inter-related mechanisms which shaped the evolution of the atmosphere, starting with the volatile sources and sinks. Going from the deep interior to the top of the atmosphere, we describe volcanic outgassing, surface-atmosphere interactions, and atmosphere escape. Furthermore, we address more complex aspects of the history of Venus, including the role of Late Accretion impacts, how magnetic field generation is tied into long-term evolution, and the implications of geochemical and geodynamical feedback cycles for atmospheric evolution. We highlight plausible end-member evolutionary pathways that Venus could have followed, from accretion to its present-day state, based on modeling and observations. In a first scenario, the planet was desiccated by atmospheric escape during the magma ocean phase. In a second scenario, Venus could have harbored surface liquid water for long periods of time, until its temperate climate was destabilized and it entered a runaway greenhouse phase. In a third scenario, Venus’s inefficient outgassing could have kept water inside the planet, where hydrogen was trapped in the core and the mantle was oxidized. We discuss existing evidence and future observations/missions required to refine our understanding of the planet’s history and of the complex feedback cycles between the interior, surface, and atmosphere that have been operating in the past, present or future of Venus.

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KW - Coupled evolution

KW - Feedback cycles

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KW - Volatile exchanges

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JO - Space Science Reviews

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The Long-Term Evolution of the Atmosphere of Venus: Processes and Feedback Mechanisms: Interior-Exterior Exchanges

Abstract

Bibliographical note

Funding

Keywords

UN SDGs

Access to Document

Persistent URL (handle)

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