No cryosphere-confined aquifer below InSight on Mars
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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.
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.
Suggested CitationManga, M., & Wright, V. (2021). No cryosphere-confined aquifer below InSight on Mars. Geophysical Research Letters, 48(8), e2021GL093127.
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