Tidal disruption of inviscid planetesimals

Details Tidal disruption of inviscid planetesimals Tidal disruption of inviscid planetesimals

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...92..165b&link_type=abstract

Icarus (ISSN 0019-1035), vol. 92, July 1991, p. 165-178. SNSF-supported research.

Computer Science

21

Protoplanets, Roche Limit, Tides, Accumulations, Angular Momentum, Planetary Mass

Scientific paper

In view of previous efforts' demonstration that strongly dissipative planetesimals are immune to tidal disruption, an examination is presently conducted of the complementary case of inviscid planetesimals arising from collisions that are sufficiently energetic to entirely melt the resulting planetesimal and debris. The tidal disruption is numerically simulated by means of the smoothed particle hydrodynamics (SPH) code of Cameron and Benz (1991), concentrating on the tidal disruption of 0.01 earth-mass planetesimals passing by the earth with variations in the impact parameter at perigee and velocity at infinity. The SPH models show that tidal forces during a close encounter can efficiently convert orbital angular momentum into spin angular momentum, thereby initiating equatorial mass-shedding to inviscid planetesimals that have been spun up beyond the limit of rotational stability.

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