Tidal torques on infrequently colliding particle disks in binary systems and the truncation of the asteroid belt

Details Tidal torques on infrequently colliding particle disks in binary systems and the truncation of the asteroid belt Tidal torques on infrequently colliding particle disks in binary systems and the truncation of the asteroid belt

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...42..271f&link_type=abstract

Icarus, vol. 42, May 1980, p. 271-280.

Astronomy and Astrophysics

Astronomy

12

Asteroid Belts, Astronomical Models, Binary Stars, Particle Collisions, Resonance, Tides, Two Body Problem, Digital Simulation, Disks (Shapes), Dynamic Stability, Eccentricity, Monte Carlo Method, Orbital Resonances (Celestial Mechanics), Torque, Asteroids, Asteroid Belt, Tidal Effects, Torques, Collisions, Mass, Disks, Particles, Reynolds Number, Orbits, Period, Gaps, Resonance, Data, Evolution, Statistical Methods, Monte Carlo Techniques, Gases, Simulations, Frequency, Inclination

Scientific paper

Conditions leading to the truncation, at the 2:1 resonance, of a disk of infrequently colliding particles surrounding the primary of a binary system are studied numerically and analytically. Attention is given to the case in which the mass ratio, q, is sufficiently small (less than about 0.1) and the radius of the disk centered on the primary allowably larger, so that first-order orbit-orbit resonances between ring material and the secondary can lie within it. Collisions are found to be less frequent than q to the -2/3 power orbital periods (the period of the forced eccentricity at the 2:1 resonance), and truncation occurs and Kirkwood gaps are produced only if the particle eccentricity is less than some critical value, estimated to be of order q to the 5/9 power, or approximately 0.02 for the sun-Jupiter case having q equal to 10 to the -3rd power.

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