COMPARING 2D AXISYMMETRIC AND 3D SPHERICAL MODELS OF MARTIAN MANTLE CONVECTION CONSTRAINED BY MELTING HISTORY

Details COMPARING 2D AXISYMMETRIC AND 3D SPHERICAL MODELS OF MARTIAN MANTLE CONVECTION CONSTRAINED BY MELTING HISTORY COMPARING 2D AXISYMMETRIC AND 3D SPHERICAL MODELS OF MARTIAN MANTLE CONVECTION CONSTRAINED BY MELTING HISTORY

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p31a1240s&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P31A-1240

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[5724] Planetary Sciences: Fluid Planets / Interiors, [6225] Planetary Sciences: Solar System Objects / Mars

Scientific paper

The timing of volcanic activity is an important constraint on the thermal evolution of Mars. While most of Tharsis rise was in place by end of the Noachian period, at least one volcano on Tharsis swell (Arsia Mons) has been active within the last 10-30 My, indicating that upwelling convective flow remains active on Mars today. This places a constraint on convection within the Martian mantle. Previous work in 2D axisymmetric geometry has shown that present day melting would be restricted to the heads of hot mantle plumes that rise from core-mantle boundary, consistent with the spatially localized distribution of recent volcanism on Mars. The existence of young volcanism on Mars implies that adiabatic decompression melting and, hence, upwelling convective flow in the mantle remains important on Mars at present. The computational grid used for previous work was an axisymmetric, hemispherical shell rather than a full, 3D spherical shell. In this work, mantle convection simulations were performed using finite element code CitcomS in 3D sphere. Comparison between 2D axisymmetry and 3D spherical convection will be presented.

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