View in EDS HTML Full Text PDF Full Text

Magma Ocean, Water, and the Early Atmosphere of Venus.

Saved in:
Bibliographic Details
Title: Magma Ocean, Water, and the Early Atmosphere of Venus.
Authors: Salvador, Arnaud1,2,3 (AUTHOR), Avice, Guillaume4 (AUTHOR), Breuer, Doris5 (AUTHOR) doris.breuer@dlr.de, Gillmann, Cédric6 (AUTHOR), Lammer, Helmut7 (AUTHOR), Marcq, Emmanuel8 (AUTHOR), Raymond, Sean N.9 (AUTHOR), Sakuraba, Haruka10 (AUTHOR), Scherf, Manuel7,11,12 (AUTHOR), Way, M. J.13,14 (AUTHOR)
Source: Space Science Reviews. Oct2023, Vol. 219 Issue 7, p1-107. 107p.
Subjects: Venusian atmosphere, Inner planets, Magmas, Venus (Planet), Long-Term Evolution (Telecommunications), Ocean
Abstract: The current state and surface conditions of the Earth and its twin planet Venus are drastically different. Whether these differences are directly inherited from the earliest stages of planetary evolution, when the interior was molten, or arose later during the long-term evolution is still unclear. Yet, it is clear that water, its abundance, state, and distribution between the different planetary reservoirs, which are intimately related to the solidification and outgassing of the early magma ocean, are key components regarding past and present-day habitability, planetary evolution, and the different pathways leading to various surface conditions. In this chapter we start by reviewing the outcomes of the accretion sequence, with particular emphasis on the sources and timing of water delivery in light of available constraints, and the initial thermal state of Venus at the end of the main accretion. Then, we detail the processes at play during the early thermo-chemical evolution of molten terrestrial planets, and how they can affect the abundance and distribution of water within the different planetary reservoirs. Namely, we focus on the magma ocean cooling, solidification, and concurrent formation of the outgassed atmosphere. Accounting for the possible range of parameters for early Venus and based on the mechanisms and feedbacks described, we provide an overview of the likely evolutionary pathways leading to diverse surface conditions, from a temperate to a hellish early Venus. The implications of the resulting surface conditions and habitability are discussed in the context of the subsequent long-term interior and atmospheric evolution. Future research directions and observations are proposed to constrain the different scenarios in order to reconcile Venus' early evolution with its current state, while deciphering which path it followed. [ABSTRACT FROM AUTHOR]
Copyright of Space Science Reviews is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Engineering Source
Full text is not displayed to guests.
FullText Links:
  – Type: pdflink
Text:
  Availability: 1
Header DbId: egs
DbLabel: Engineering Source
An: 173321798
AccessLevel: 6
PubType: Academic Journal
PubTypeId: academicJournal
PreciseRelevancyScore: 0
IllustrationInfo
Items – Name: Title
  Label: Title
  Group: Ti
  Data: Magma Ocean, Water, and the Early Atmosphere of Venus.
– Name: Author
  Label: Authors
  Group: Au
  Data: <searchLink fieldCode="AR" term="%22Salvador%2C+Arnaud%22">Salvador, Arnaud</searchLink><relatesTo>1,2,3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Avice%2C+Guillaume%22">Avice, Guillaume</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Breuer%2C+Doris%22">Breuer, Doris</searchLink><relatesTo>5</relatesTo> (AUTHOR)<i> doris.breuer@dlr.de</i><br /><searchLink fieldCode="AR" term="%22Gillmann%2C+Cédric%22">Gillmann, Cédric</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Lammer%2C+Helmut%22">Lammer, Helmut</searchLink><relatesTo>7</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Marcq%2C+Emmanuel%22">Marcq, Emmanuel</searchLink><relatesTo>8</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Raymond%2C+Sean+N%2E%22">Raymond, Sean N.</searchLink><relatesTo>9</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Sakuraba%2C+Haruka%22">Sakuraba, Haruka</searchLink><relatesTo>10</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Scherf%2C+Manuel%22">Scherf, Manuel</searchLink><relatesTo>7,11,12</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Way%2C+M%2E+J%2E%22">Way, M. J.</searchLink><relatesTo>13,14</relatesTo> (AUTHOR)
– Name: TitleSource
  Label: Source
  Group: Src
  Data: <searchLink fieldCode="JN" term="%22Space+Science+Reviews%22">Space Science Reviews</searchLink>. Oct2023, Vol. 219 Issue 7, p1-107. 107p.
– Name: Subject
  Label: Subjects
  Group: Su
  Data: <searchLink fieldCode="DE" term="%22Venusian+atmosphere%22">Venusian atmosphere</searchLink><br /><searchLink fieldCode="DE" term="%22Inner+planets%22">Inner planets</searchLink><br /><searchLink fieldCode="DE" term="%22Magmas%22">Magmas</searchLink><br /><searchLink fieldCode="DE" term="%22Venus+%28Planet%29%22">Venus (Planet)</searchLink><br /><searchLink fieldCode="DE" term="%22Long-Term+Evolution+%28Telecommunications%29%22">Long-Term Evolution (Telecommunications)</searchLink><br /><searchLink fieldCode="DE" term="%22Ocean%22">Ocean</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: The current state and surface conditions of the Earth and its twin planet Venus are drastically different. Whether these differences are directly inherited from the earliest stages of planetary evolution, when the interior was molten, or arose later during the long-term evolution is still unclear. Yet, it is clear that water, its abundance, state, and distribution between the different planetary reservoirs, which are intimately related to the solidification and outgassing of the early magma ocean, are key components regarding past and present-day habitability, planetary evolution, and the different pathways leading to various surface conditions. In this chapter we start by reviewing the outcomes of the accretion sequence, with particular emphasis on the sources and timing of water delivery in light of available constraints, and the initial thermal state of Venus at the end of the main accretion. Then, we detail the processes at play during the early thermo-chemical evolution of molten terrestrial planets, and how they can affect the abundance and distribution of water within the different planetary reservoirs. Namely, we focus on the magma ocean cooling, solidification, and concurrent formation of the outgassed atmosphere. Accounting for the possible range of parameters for early Venus and based on the mechanisms and feedbacks described, we provide an overview of the likely evolutionary pathways leading to diverse surface conditions, from a temperate to a hellish early Venus. The implications of the resulting surface conditions and habitability are discussed in the context of the subsequent long-term interior and atmospheric evolution. Future research directions and observations are proposed to constrain the different scenarios in order to reconcile Venus' early evolution with its current state, while deciphering which path it followed. [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Space Science Reviews is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
PLink https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=egs&AN=173321798
RecordInfo BibRecord:
  BibEntity:
    Identifiers:
      – Type: doi
        Value: 10.1007/s11214-023-00995-7
    Languages:
      – Code: eng
        Text: English
    PhysicalDescription:
      Pagination:
        PageCount: 107
        StartPage: 1
    Subjects:
      – SubjectFull: Venusian atmosphere
        Type: general
      – SubjectFull: Inner planets
        Type: general
      – SubjectFull: Magmas
        Type: general
      – SubjectFull: Venus (Planet)
        Type: general
      – SubjectFull: Long-Term Evolution (Telecommunications)
        Type: general
      – SubjectFull: Ocean
        Type: general
    Titles:
      – TitleFull: Magma Ocean, Water, and the Early Atmosphere of Venus.
        Type: main
  BibRelationships:
    HasContributorRelationships:
      – PersonEntity:
          Name:
            NameFull: Salvador, Arnaud
      – PersonEntity:
          Name:
            NameFull: Avice, Guillaume
      – PersonEntity:
          Name:
            NameFull: Breuer, Doris
      – PersonEntity:
          Name:
            NameFull: Gillmann, Cédric
      – PersonEntity:
          Name:
            NameFull: Lammer, Helmut
      – PersonEntity:
          Name:
            NameFull: Marcq, Emmanuel
      – PersonEntity:
          Name:
            NameFull: Raymond, Sean N.
      – PersonEntity:
          Name:
            NameFull: Sakuraba, Haruka
      – PersonEntity:
          Name:
            NameFull: Scherf, Manuel
      – PersonEntity:
          Name:
            NameFull: Way, M. J.
    IsPartOfRelationships:
      – BibEntity:
          Dates:
            – D: 01
              M: 10
              Text: Oct2023
              Type: published
              Y: 2023
          Identifiers:
            – Type: issn-print
              Value: 00386308
          Numbering:
            – Type: volume
              Value: 219
            – Type: issue
              Value: 7
          Titles:
            – TitleFull: Space Science Reviews
              Type: main
ResultId 1