Tidal Distortion and Disruption of Earth-Crossing Asteroids

Details Tidal Distortion and Disruption of Earth-Crossing Asteroids Tidal Distortion and Disruption of Earth-Crossing Asteroids

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998icar..134...47r&link_type=abstract

Icarus, Volume 134, Issue 1, pp. 47-76.

Statistics

Applications

80

Scientific paper

We present results of numerical simulations that show that Earth's tidal forces can both distort and disrupt Earth-crossing asteroids that have weak ``rubble-pile'' structures. Building on previous studies, we consider more realistic asteroid shapes and trajectories, test a variety of spin rates and axis orientations, and employ a dissipation algorithm to treat more accurately collisions between the particles that make up the model asteroid. We explore a large parameter space, including the asteroid's periapse q, encounter velocity with the Earth v_∞, spin period P, initial spin axis orientation, and body orientation at periapse. We parameterize the simulation outcomes by the amount of mass stripped from the asteroid during a flyby. Our most severe disruptions result in fragment trains similar in character to the ``string of pearls'' created when Comet D/Shoemaker-Levy 9 was disrupted near Jupiter in 1992. Less catastrophic disruptions cause material to be stripped off in more isotropic fashion, leaving a central remnant with a characteristic distorted shape. Some ejecta can enter into stable orbits around the remnant, creating a binary or multiple system. Even when no mass is lost tidal forces and torques can modify the asteroid's shape and spin. Our results show that mass loss is enhanced for small values of q, v_∞, and P, and depends to a certain extent on the body's initial spin orientation (for example, retrograde rotation reduces mass loss). An elongated asteroid was found to be far easier to disrupt than a spherical one, though the orientation of the ellipsoid at periapse can noticeably change the outcome. The size and orbital distribution of the ejecta are discussed, along with the applications of this technique towards an understanding of doublet craters, crater chains, and asteroids with peculiar shapes and spins.

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