No cryosphere-confined aquifer below InSight on Mars

dc.contributor.author Manga, Michael
dc.contributor.author Wright, Vanshan
dc.date.accessioned 2021-12-16T20:58:31Z
dc.date.available 2021-12-16T20:58:31Z
dc.date.issued 2021-04-11
dc.description Author Posting. © American Geophysical Union, 2021. This article is posted here by permission of American Geophysical Union for personal use, not for redistribution. The definitive version was published in Geophysical Research Letters 48(8), (2021): e2021GL093127, https://doi.org/10.1029/2021GL093127. en_US
dc.description.abstract The seismometer deployed by the InSight lander measured the seismic velocity of the Martian crust. We use a rock physics model to interpret those velocities and constrain hydrogeological properties. The seismic velocity of the upper ∼10 km is too low to be ice-saturated. Hence there is no cryosphere that confines deeper aquifers and possibly no aquifers locally. An increase in seismic velocity at depths of ∼10 km could be explained by a few volume percent of mineral cement (1%–5%) in pore space and may document the past depth of aquifers. en_US
dc.description.sponsorship M. Manga was supported by NASA grant 80NSSC19K0545. en_US
dc.identifier.citation Manga, M., & Wright, V. (2021). No cryosphere-confined aquifer below InSight on Mars. Geophysical Research Letters, 48(8), e2021GL093127. en_US
dc.identifier.doi 10.1029/2021GL093127
dc.identifier.uri https://hdl.handle.net/1912/27823
dc.publisher American Geophysical Union en_US
dc.relation.uri https://doi.org/10.1029/2021GL093127
dc.subject Cryosphere en_US
dc.subject Marsquakes en_US
dc.subject Rock physics en_US
dc.title No cryosphere-confined aquifer below InSight on Mars en_US
dc.type Article en_US
dspace.entity.type Publication
relation.isAuthorOfPublication c26ef2b3-5aaa-4f94-afd9-e40d0468488a
relation.isAuthorOfPublication 7d3d9e58-1e4c-475f-a4a7-a8e4ddb4bbf8
relation.isAuthorOfPublication.latestForDiscovery c26ef2b3-5aaa-4f94-afd9-e40d0468488a
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