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Pre-mission InSights on the Interior of Mars

Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman and Banerdt, W. Bruce and Breuer, Doris and Christensen, Ulrich and Dehant, Véronique and Drilleau, Mélanie and Folkner, William and Fuji, Nobuaki and Garcia, Raphaël F. and Giardini, Domenico and Golombek, Matthew P. and Grott, Matthias and Gudkova, Tamara and Johnson, Catherine and Khan, Amir and Langlais, Benoit and Mittelholz, Anna and Mocquet, Antoine and Myhill, Robert and Panning, Mark and Perrin, Clément and Pike, Tom and Plesa, Ana-Catalina and Rivoldini, Attilio and Samuel, Henri and Stähler, Simon C. and van Driel, Martin and Van Hoolst, Tim and Verhoeven, Olivier and Weber, Renee and Wieczorek, Mark Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (3). 1-72. ISSN 0038-6308

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Official URL: https://doi.org/10.1007/s11214-018-0563-9

Abstract

Abstract The Interior exploration using Seismic Investigations, Geodesy, and Heat Trans- port (InSight) Mission will focus on Mars’ interior structure and evolution. The basic structure of crust, mantle, and core form soon after accretion. Understanding the early differentiation process on Mars and how it relates to bulk composition is key to improving our understanding of this process on rocky bodies in our solar system, as well as in other solar systems. Current knowledge of differentiation derives largely from the layers observed via seismology on the Moon. However, the Moon’s much smaller diameter make it a poor analog with respect to interior pressure and phase changes. In this paper we review the current knowledge of the thickness of the crust, the diameter and state of the core, seismic attenuation, heat flow, and interior composition. InSight will conduct the first seismic and heat flow measurements of Mars, as well as more precise geodesy. These data reduce uncertainty in crustal thickness, core size and state, heat flow, seismic activity and meteorite impact rates by a factor of 3–10× relative to previous estimates. Based on modeling of seismic wave propagation, we can further constrain interior temperature, composition, and the location of phase changes. By combining heat flow and a well constrained value of crustal thickness, we can estimate the distribution of heat producing elements between the crust and mantle. All of these quantities are key inputs to models of interior convection and thermal evolution that predict the processes that control subsurface temperature, rates of volcanism, plume distribution and stability, and convective state. Collectively these factors offer strong controls on the overall evolution of the geology and habitability of Mars.

Item Type:Article
HAL Id:hal-01990798
Audience (journal):International peer-reviewed journal
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Institution:Université de Toulouse > Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
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Deposited By: Raphael Garcia
Deposited On:23 Jan 2019 13:00

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