Mantle Plumes on Venus: Implications for Mantle Viscosity, Water Content, and Melting

Details Mantle Plumes on Venus: Implications for Mantle Viscosity, Water Content, and Melting Mantle Plumes on Venus: Implications for Mantle Viscosity, Water Content, and Melting

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1885s&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1885

Physics

Scientific paper

Gravity, topography, and VIRTIS emissivity suggests the presence of ~10 deep, active mantle plumes on Venus. This study predicts the number of plumes formed at the core-mantle boundary (CMB), their characteristics, and the amount of partial melt using 3D spherical simulations with large viscosities variations and internal heating. The case with the most realistic lid thickness and internal heating (3.3 TW) has a mantle viscosity of 1020 Pa s, and a mantle temperature difference of 1140°K, but predicts more than 70 plumes globally. Since wet melting is predicted over much of the upper mantle, over time it may have lost significant volatiles. Assuming 100 ppm water in the mantle, 10 plumes erupting for 200 m.y. will outgas approximately the amount of water in the lower atmosphere. A higher level of internal heating may be required to achieve simulations with ~10 plumes and a thinner lid. Alternatively, if the mantle is heating up due to the stagnant lid, the effect is equivalent to having lower rates of internal heating.

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