Tidal disruption of viscous bodies

Details Tidal disruption of viscous bodies Tidal disruption of viscous bodies

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992icar...95...86s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 95, Jan. 1992, p. 86-99. Research supported by NSERC.

Statistics

Computation

44

Celestial Mechanics, Computational Fluid Dynamics, Protoplanets, Tides, Viscous Fluids, Astronomical Models, Equations Of Motion, Planetary Evolution, Poisson Equation

Scientific paper

Tidal disruptions are investigated in viscous-fluid planetesimals whose radius is small relative to the distance of closest (parabolic-orbit) approach to a planet. The planetesimal surface is in these conditions always ellipsoidal, facilitating treatment by coupled ODEs which are solvable with high accuracy. While the disrupted planetesimals evolve into needlelike ellipsoids, their density does not decrease. The validity of viscous fluid treatment holds for solid (ice or rock) planetesimals in cases where tidal stresses are greater than material strength, but integrity is maintained by self-gravity.

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