Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974icar...22..436h&link_type=abstract
Icarus, vol. 22, Aug. 1974, p. 436-447.
Astronomy and Astrophysics
Astronomy
13
Asteroids, Binary Stars, Extrasolar Planets, Planetary Evolution, Solar System, Astronomical Models, Coalescing, Collision Parameters, Jupiter (Planet), Long Term Effects, Nebulae, Planetary Systems
Scientific paper
A theory is presented for determining regions where planets may form in binary star systems. Planet formation by accretion is assumed possible if mean planetesimal collision velocities do not exceed a critical value. A general feature of planetary systems in binary stars is the existence of two zones. The inner zone has enough damping to permit unimpeded growth by accretion; in the outer zone, growth proceeds to a limited diameter, beyond which damping is insufficient. It is shown that the asteroids could not have failed to coalesce due to Jupiter perturbations in the primitive solar nebula. Binary star systems with semimajor axis less than 30 AU are not likely to have planets; these include Alpha Centauri and 70 Ophiuchi. Systems possibly possessing planets include Eta Cassiopeiae, 40 Eridani, and Sigma 2398. Epsilon Eridani is a marginal case.
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