Models of evolutionary tracks of planetary satellites

Details Models of evolutionary tracks of planetary satellites Models of evolutionary tracks of planetary satellites

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...209..411h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 209, no. 1-2, Jan. 1989, p. 411-422.

Astronomy and Astrophysics

Astrophysics

2

Astronomical Models, Capture Effect, Natural Satellites, Planetary Evolution, Planets, Protoplanets, Collisions, Orbital Mechanics, Planetary Gravitation, Planetary Rings, Planetary Rotation, Planets, Satellites, Models, Evolution, Origin, Formation, Accretion, Planetesimals, Capture, Collisions, Rings, Parameters, Jupiter, Saturn, Uranus, Mass, Velocity, Eccentricity, Calculations, Earth, Moon, Phobos, Io, Mimas, Oberon, Triton, Amalthea, Density, Hypotheses

Scientific paper

Satellite formation is studied within the scenario of collisional capture of planetesimal by an accreting planet. The capture probability of planetary satellites by free-free and bound-free collisions among planetesimals within the planet's gravitational sphere of action is calculated. The possiblility of satellite formation by near-grazing and/or destructive collisions between a planetesimal and the planet itself is discussed. A capture criterion for satellite formation by collisions between planetesimals is formulated. After capture the satellite evolves by coaccretion, being eventually crushed by collisions with heliocentric planetesimals, forming subsequently a circumplanetary ring. Evolutionary tracks for selected satellites formed by coaccretion, or accreting in circumplanetary rings are calculated. The surface density in the satellite systems of Jupiter, Saturn, and Uranus is determined, masses, velocities, eccentricites and formation intervals being shown for selected satellites.

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