Melting and differentiation in Venus with a cold start: A mechanism of the thin crust formation

Details Melting and differentiation in Venus with a cold start: A mechanism of the thin crust formation Melting and differentiation in Venus with a cold start: A mechanism of the thin crust formation

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789..117s&link_type=abstract

In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 117-118 (SEE N93-14288 04-91)

Computer Science

Melting, Planetary Crusts, Planetary Evolution, Plates (Tectonics), Venus (Planet), Venus Surface, Basalt, Tectonics, Thickness

Scientific paper

Recent works argue that the venusian crust is thin: less than 10-30 km. However, any convective model of Venus unavoidably predicts melting and a fast growth of the basaltic crust, up to its maximum thickness of about 70 km limited, by the gabbro-eclogite phase transition. The crust is highly buoyant due to both its composition and temperature and it is problematic to find a mechanism providing its effective recycling and thinning in the absence of plate tectonics. There are different ways to solve this contradiction. This study suggests that a thin crust can be produced during the entire evolution of Venus if Venus avoided giant impacts.

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