2D Two-fluid Simulations of Core Formation in 10km Planetesimals

Details 2D Two-fluid Simulations of Core Formation in 10km Planetesimals 2D Two-fluid Simulations of Core Formation in 10km Planetesimals

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmmr43b1877m&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #MR43B-1877

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[0545] Computational Geophysics / Modeling, [5724] Planetary Sciences: Fluid Planets / Interiors

Scientific paper

In the early solar system, planetesimals differentiated within the first few million years after the formation of the solar system due to extreme heating from 26Al and other possible sources. To study the dynamics of this differentiation process, we simulate a fully fluid body, 10 kilometers in diameter, using a simple two-dimensional two-fluid model. The silicate convection is simulated with an Eulerian spectral method in longitude and radius; whereas the iron is advected using a Lagrangian particle method. Our simulations show the competition between the turbulent advection and the gravitational settling of the iron in the density-stratified rotating, convecting body.

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