An evaluation of convective instability in homogeneous terrestrial planet models

Details An evaluation of convective instability in homogeneous terrestrial planet models An evaluation of convective instability in homogeneous terrestrial planet models

Jul 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979izssr.......73s&link_type=abstract

Akademiia Nauk SSSR, Izvestiia, Fizika Zemli, July 1979, p. 73-77. In Russian.

Astronomy and Astrophysics

Astronomy

Astronomical Models, Convection, Planetary Structure, Terrestrial Planets, Mars (Planet), Mercury (Planet), Planetary Cores, Planetary Mantles, Venus (Planet), Viscosity

Scientific paper

Convection in terrestrial planet interiors is calculated on the basis of a planetary model with an inhomogeneous viscosity distribution, a well-defined core and mantle and a uniform heat-source distribution. Small perturbations in the initial equilibrium conditions are expressed in an eigenvalue problem which is solved for the minimum Rayleigh number at which convection will occur and for the distributions of velocity and temperature perturbations with planetary radius. It is noted that, according to the model, all the terrestrial planets exhibit convective instability with the exception of Mercury, due to its high effective viscosity. Mantle convection in the moon and Mars is shown to develop under a thick, immovable outer shell, making surface evidence of convection unlikely, while convection in the earth and Venus is found to be essentially similar except for the lower critical Rayleigh number of Venus.

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