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Star-Disc Interactions and Binary Formation

Published online by Cambridge University Press:  12 April 2016

Cathie Clarke
Cathie Clarke*
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA, U.K.

Extract

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By the time a binary arrives on the main sequence, its dynamics have essentially become those of a simple two-body system, so that its orbital parameters are constants of the motion thereafter. This statement of course needs to be modified under several circumstances, such as where tidal effects, mass exchange or interactions with field stars come into play. For the majority of binaries, however, orbital evolution is all but over by the main sequence. Therefore, in order to explain the distribution of binary orbital parameters one has to look to earlier times (prior to 107 years) when the more complicated dynamics can drive the orbital evolution that establishes these parameters.

Type
Theoretical Aspects
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 176 - 184
Copyright
Copyright © Astronomical Society of the Pacific 1992

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