Binary formation

Details Binary formation Binary formation

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983pazh....9..160t&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 9, Mar. 1983, p. 160-165) Soviet Astronomy Letters (ISSN 0360-0327), vol. 9, Mar.-Apr.

Astronomy and Astrophysics

Astronomy

5

Binary Stars, Protostars, Stellar Evolution, Cosmic Dust, Interstellar Gas, Stellar Mass Accretion, Stellar Models

Scientific paper

The early evolutionary stages of a single protostar are examined analytically, and the results are applied to study the rotational fragmentation of a collapsing gas-dust cloud. Two types of binary systems can form in this manner. Wide pairs (alpha systems, P/orb/ approximately equal to or greater than 100 yr), generally with components of unequal mass, will develop before a hydrostatic-equilibrium gas-dust core is able to form. Close pairs (beta systems, P/orb/ approximately equal to or less than 100 yr), whose components usually are nearly equal in mass, will originate after the gas-dust core has formed and proceeds to collapse.

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