Isostatic gravity and elastic bending models of Olympus Mons, Mars

Details Isostatic gravity and elastic bending models of Olympus Mons, Mars Isostatic gravity and elastic bending models of Olympus Mons, Mars

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986angeo...4..537j&link_type=abstract

Annales Geophysicae, Series B - Terrestrial and Planetary Physics (ISSN 0755-0685), vol. 4, Oct. 1986, p. 537-546. DFG-supported

Physics

5

Gravitational Effects, Lithosphere, Mars Surface, Planetary Crusts, Planetary Mantles, Volcanology, Elastic Bending, Isostatic Pressure, Mars Photographs, Topography

Scientific paper

Gravity models of Olympus Mons, Mars are presented using Wu et al.'s (1984) new higher volume estimate of the mountain. Airy compensation models are shown to give mean crustal thicknesses (T) between 30 and 300 km. When the thickness of the root is added to the T upper limit, a 400-km depth of compensation is obtained. A totally compensated Pratt model is found to give an 800-km depth of compensation. Assuming the Airy roots of the gravity models to be caused by bending of the lithosphere, elastic bending models further restrict the range of T (30-150 km), and give boundaries for the lithosphere thickness, the Young's modulus, and the flexural rigidity.

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