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Seismic wave detectability on Venus using ground deformation sensors, infrasound sensors on balloons and airglow imagers
  • +15
  • Raphael F. Garcia,
  • Iris van Zelst,
  • Taichi Kawamura,
  • Sven Peter Näsholm,
  • Anna Catherine Horleston,
  • Sara Klaasen,
  • Maxence Lefevre,
  • Céline Marie Solberg,
  • Krystyna T. Smolinski,
  • Ana-Catalina Plesa,
  • Quentin Brissaud,
  • Julia S. Maia,
  • Simon C. Stähler,
  • Philippe Lognonné,
  • Mark Paul Panning,
  • Anna Gülcher,
  • Richard Ghail,
  • Barbara De Toffoli
Raphael F. Garcia
Institut Supérieur de l'Aéronautique et de l'Espace, ISAE-SUPAERO

Corresponding Author:[email protected]

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Iris van Zelst
German Aerospace Center
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Taichi Kawamura
Université Paris Cité, Institut de physique du globe de Paris, CNRS
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Sven Peter Näsholm
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Anna Catherine Horleston
University of Bristol
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Sara Klaasen
Swiss Federal Institute of Technology in Zurich
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Maxence Lefevre
Sorbonne Université
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Céline Marie Solberg
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Krystyna T. Smolinski
ETH Zürich
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Ana-Catalina Plesa
German Aerospace Center
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Quentin Brissaud
Norwegian Seismic Array (NORSAR)
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Julia S. Maia
DLR DLR Institute of Planetary Research
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Simon C. Stähler
Eidgenössische Technische Hochschule Zürich
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Philippe Lognonné
Université Paris Cité, Institute de physique de globe de Paris, CNRS
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Mark Paul Panning
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Anna Gülcher
California Institute of Technology; NASA Jet Propulsion Laboratory; ETH Zürich
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Richard Ghail
Royal Holloway University of London
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Barbara De Toffoli
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The relatively unconstrained internal structure of Venus is a missing piece in our understanding of the Solar System formation and evolution. To determine the seismic structure of Venus’ interior, the detection of seismic waves generated by venusquakes is crucial, as recently shown by the new seismic and geodetic constraints on Mars’ interior obtained by the InSight mission. In the next decades multiple missions will fly to Venus to explore its tectonic and volcanic activity, but they will not be able to conclusively report on seismicity or detect actual seismic waves.
Looking towards the next fleet of Venus missions in the future, various concepts to measure seismic waves have already been explored in the past decades. These detection methods include typical geophysical ground sensors already deployed on Earth, the Moon, and Mars; pressure sensors on balloons; and airglow imagers on orbiters to detect ground motion, the infrasound signals generated by seismic waves, and the corresponding airglow variations in the upper atmosphere.
Here, we provide a first comparison between the detection capabilities of these different measurement techniques and recent estimates of Venus’ seismic activity.
In addition, we discuss the performance requirements and measurement durations required to detect seismic waves with the various detection methods. As such, our study clearly presents the advantages and limitations of the different seismic wave detection techniques and can be used to drive the design of future mission concepts aiming to study the seismicity of Venus.
10 Apr 2024Submitted to ESS Open Archive
11 Apr 2024Published in ESS Open Archive