Star-Disc Interactions and Binary Formation
1992 ◽
Vol 135
◽
pp. 176-184
Keyword(s):
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.
Keyword(s):
1992 ◽
Vol 135
◽
pp. 30-40
Keyword(s):
2019 ◽
Vol 626
◽
pp. A128
◽
2021 ◽
Vol 503
(1)
◽
pp. 1233-1247
1989 ◽
Vol 106
◽
pp. 234-234
Keyword(s):
1992 ◽
Vol 151
◽
pp. 21-30
1992 ◽
Vol 152
◽
pp. 329-332