Study of physical properties of spectroscopic binary stars |
| |
| Authors: | E I Popova A V Tutukov L R Yungelson |
| |
| Institution: | 1. Astronomical Council, U.S.S.R. Academy of Sciences, Moscow, U.S.S.R.
|
| |
| Abstract: | The main results of a study of a catalogue of physical parameters of 1041 spectroscopic binaries are presented. The distribution of spectroscopic binaries over all main parametersM 1, a, e, M1/M2, P, and certain dependencies between some of them have been found. - It appears that among bright (m v?3 m –5 m ) stars withM?1M ⊙, about 40% are apparently spectroscopic binaries with comparable masses of components.
- The majority of spectroscopic binaries with the ratio of the large semiaxis of the orbit to the radius of the primarya/R 1?20, have eccentricities close to zero. This is probably a consequence of the tidal circularization of orbits of close binaries by viscous friction.
- The discovery of duplicity of double-line spectroscopic binaries is possible only if the semiamplitude of radial velocityK 1 is almost 10 times higher than the semiamplitude of the radial velocity of a single-line spectroscopic binary of the same mass.
- Double-line spectroscopic binaries witha/R ⊙?6(M 1/M ⊙)1/3,M 1≈M 2?1.5M ⊙ are almost almost absent, and the number of stars witha/R ⊙?6(M 1/M ⊙)1/3,M 1≈1.5M ⊙ is relatively low.
- The distribution of unevolved SB stars over the large semiaxis may be described by the expression d(N d/Nt)≈0.2 d loga for 6(M 1/M ⊙)1/3?a/R ⊙?100.
- The intial mass-function for primaries of spectroscopic binaries is the same Salpeter function dN d≈M 1 ?2.35 dM 1 for 1?M 1/M ⊙?30.
- It is possible to explain the observed ratio of the number of single-line spectroscopic binaries to the number of double-line binaries if one assumes that the average initial mass ratio is close to 1 and that the mass of the postmass-exchange remnant of the primary exceeds the theoretical one and/or that half of the angular momentum of the system is lost during mass-exchange.
- The above-mentioned distributions ofM 1 anda and assumptions on the mass of remnant and/or momentum loss also allow us to explain the observed shapes of dN/dM, dN/dq, and dN/da distributions after some selection effects are taken into account.
|
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
