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The Mantle Viscosity Structure of Venus

Maia, Julia and Wieczorek, M. and Plesa, Ana-Catalina (2023) The Mantle Viscosity Structure of Venus. 54th Lunar and Planetary Science Conference 2023, The Woodlands, Texas, USA.

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Official URL: https://www.hou.usra.edu/meetings/lpsc2023/pdf/1737.pdf


It is broadly accepted that Venus is a geologically active world, presenting signs of recent volcanism and tectonism [e.g., 1,2]. Yet, its interior structure and dynamics are poorly understood. One of the most informative ways of investigating Venus’s interior is to jointly analyze gravity and topography data. The initial gravity and topography studies of Venus that made use of the Pioneer Venus and later Magellan data revealed unique properties of the planet’s interior. The gravity-topography correlations for long wavelengths are considerably higher than for Earth [3]. In addition, the global apparent depth of compensation is quite large, over 100 km [4]. Taking these characteristics into account, along with the observed wavelength dependent gravity-topography, the so-called spectral admittance, [4] concluded that the long-wavelength topography of the planet was supported through mantle flows, which is commonly referred to as dynamic or active support. Several gravity and topography investigations of Venus were perform with the goal of better understanding its mantle properties. Many of these made use of the dynamic loading model developed by Hager and Clayton (1989) [5]. This model predicts the dynamic gravity and topography for a given density anomaly distribution in the mantle and a specified radial viscosity profile. Some studies [e.g., 6] focused on estimating the spatial distribution of density anomalies within the mantle, which supported the interpretation that volcanic rises are associated with mantle upwellings. Alternatively, other studies [4,7,8,9] were interested in investigating the planet’s mantle viscosity structure. We present a new investigation of the dynamic gravity and topography signatures on Venus making use of a multitaper spectral localization technique and a Bayesian inversion approach in order to provide new constraints to the mantle viscosity structure of our sister planet. The analysis is done with the VenusTopo719 topography model [10] and the MGNP180U gravity solution [11], both derived from the final Magellan mission datasets.

Item URL in elib:https://elib.dlr.de/196815/
Document Type:Conference or Workshop Item (Speech)
Title:The Mantle Viscosity Structure of Venus
AuthorsInstitution or Email of AuthorsAuthor's ORCID iDORCID Put Code
Maia, JuliaObservatoire de la Côte d’Azur, Laboratoire Lagrange, Université Côte d’Azur, Nice, Francehttps://orcid.org/0000-0002-3605-6554UNSPECIFIED
Wieczorek, M.Département de Géophysique Spatiale et Planétaire/UMR7096-CNRS, Institut de Physique du Globe de Paris, 4 Avenue de Neptune,UNSPECIFIEDUNSPECIFIED
Plesa, Ana-CatalinaUNSPECIFIEDhttps://orcid.org/0000-0003-3366-7621UNSPECIFIED
Refereed publication:No
Open Access:No
Gold Open Access:No
In ISI Web of Science:No
Page Range:p. 1737
Series Name:LPI Contribution
Keywords:Venus, Mantle Viscosity, Gravity, Topography
Event Title:54th Lunar and Planetary Science Conference 2023
Event Location:The Woodlands, Texas, USA
Event Type:international Conference
HGF - Research field:Aeronautics, Space and Transport
HGF - Program:Space
HGF - Program Themes:Space Exploration
DLR - Research area:Raumfahrt
DLR - Program:R EW - Space Exploration
DLR - Research theme (Project):R - Exploration of the Solar System, R - Planetary Evolution and Life, R - Veritas, R - Project EnVision
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Physics
Deposited By: Plesa, Dr. Ana-Catalina
Deposited On:31 Aug 2023 15:56
Last Modified:31 Aug 2023 15:56

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