Isostatic equilibrium in spherical coordinates and implications for crustal thickness on the Moon, Mars, Enceladus, and elsewhere
Isostatic equilibrium is commonly defined as the state achieved when there are no lateral gradients in hydrostatic pressure, and thus no lateral flow, at depth within the lower viscosity mantle that underlies a planetary body's outer crust. In a constant-gravity Cartesian framework, this defini...
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| Language: | en |
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AMER GEOPHYSICAL UNION
2017
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| Online Access: | http://hdl.handle.net/10150/625778 http://arizona.openrepository.com/arizona/handle/10150/625778 |