Tidal disruption of inviscid protoplanets

Details Tidal disruption of inviscid protoplanets Tidal disruption of inviscid protoplanets

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept..444b&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 444-445 (SEE N92-10728 01-91)

Computer Science

Numerical Analysis

Computer Programs, Mathematical Models, Planetary Evolution, Protoplanets, Roche Limit, Tides, Viscosity, Collisions, Computerized Simulation, Hydrodynamics, Iron, Numerical Analysis, Planetary Cores, Silicates

Scientific paper

Roche showed that equilibrium is impossible for a small fluid body synchronously orbiting a primary within a critical radius now termed the Roche limit. Tidal disruption of orbitally unbound bodies is a potentially important process for planetary formation through collisional accumulation, because the area of the Roche limit is considerably larger then the physical cross section of a protoplanet. Several previous studies were made of dynamical tidal disruption and different models of disruption were proposed. Because of the limitation of these analytical models, we have used a smoothed particle hydrodynamics (SPH) code to model the tidal disruption process. The code is basically the same as the one used to model giant impacts; we simply choose impact parameters large enough to avoid collisions. The primary and secondary both have iron cores and silicate mantles, and are initially isothermal at a molten temperature. The conclusions based on the analytical and numerical models are summarized.

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