000005876 001__ 5876
000005876 005__ 20221028113233.0
000005876 0247_ $$2DOI$$a10.1029/2022JE007298
000005876 037__ $$aSCART-2022-0108
000005876 100__ $$aWieczorek, Mark A. 
000005876 245__ $$aInSight Constraints on the Global Character of the Martian Crust
000005876 260__ $$c2022
000005876 520__ $$aAnalyses of seismic data from the InSight mission have provided the first in situ constraints on the thickness of the crust of Mars. These crustal thickness constraints are currently limited to beneath the lander that is located in the northern lowlands, and we use gravity and topography data to construct global crustal thickness models that satisfy the seismic data. These models consider a range of possible mantle and core density profiles, a range of crustal densities, a low-density surface layer, and the possibility that the crustal density of the northern lowlands is greater than that of the southern highlands. Using the preferred InSight three-layer seismic model of the crust, the average crustal thickness of the planet is found to lie between 30 and 72 km. Depending on the choice of the upper mantle density, the maximum permissible density of the northern lowlands and southern highlands crust is constrained to be between 2,850 and 3,100 kg m?3. These crustal densities are lower than typical Martian basaltic materials and are consistent with a crust that is on average more felsic than the materials found at the surface. We argue that a substantial portion of the crust of Mars is a primary crust that formed during the initial differentiation of the planet. Various hypotheses for the origin of the observed intracrustal seisimic layers are assessed, with our preferred interpretation including thick volcanic deposits, ejecta from the Utopia basin, porosity closure, and differentiation products of a Borealis impact melt sheet.
000005876 536__ $$a3PRODPLANINT/$$c3PRODPLANINT/$$f3PRODPLANINT
000005876 594__ $$aNO
000005876 700__ $$aBroquet, Adrien 
000005876 700__ $$aMcLennan, Scott M. 
000005876 700__ $$aRivoldini, Attilio 
000005876 700__ $$aGolombek, Matthew 
000005876 700__ $$aAntonangeli, Daniele 
000005876 700__ $$aBeghein, Caroline 
000005876 700__ $$aGiardini, Domenico 
000005876 700__ $$aGudkova, Tamara 
000005876 700__ $$aGyalay, Szilárd 
000005876 700__ $$aJohnson, Catherine L. 
000005876 700__ $$aJoshi, Rakshit 
000005876 700__ $$aKim, Doyeon 
000005876 700__ $$aKing, Scott D. 
000005876 700__ $$aKnapmeyer-Endrun, Brigitte 
000005876 700__ $$aLognonné, Philippe 
000005876 700__ $$aMichaut, Chloé 
000005876 700__ $$aMittelholz, Anna 
000005876 700__ $$aNimmo, Francis 
000005876 700__ $$aOjha, Lujendra 
000005876 700__ $$aPanning, Mark P. 
000005876 700__ $$aPlesa, Ana-Catalina 
000005876 700__ $$aSiegler, Matthew A. 
000005876 700__ $$aSmrekar, Suzanne E. 
000005876 700__ $$aSpohn, Tilman 
000005876 700__ $$aBanerdt, W. Bruce
000005876 773__ $$n5$$pJournal of Geophysical Research: Planets$$v127$$y2022
000005876 8560_ $$fattilio.rivoldini@observatoire.be
000005876 8564_ $$s2053358$$uhttp://publi2-as.oma.be/record/5876/files/Wieczorek2022ta12.pdf
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000005876 905__ $$apublished in
000005876 980__ $$aREFERD