Apsidal motion in main-sequence binary stars

Details Apsidal motion in main-sequence binary stars Apsidal motion in main-sequence binary stars

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.207..323j&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 207, March 15, 1984, p. 323-337.

Astronomy and Astrophysics

Astronomy

52

Apsides, Binary Stars, Main Sequence Stars, Stellar Evolution, Stellar Motions, Stellar Mass, Stellar Models

Scientific paper

The apsidal motion constant has been computed for models of evolving main-sequence stars. The behavior of the apsidal constant during main-sequence evolution is verified by observations. Monet's method for studying apsidal motion in spectroscopic binary systems has been extended. In addition to resolving many of the discrepancies between theory and observation of apsidal motion, a method is presented for estimating the masses and ages of binary systems from the spectral type of the primary and the observed apsidal motion (if present). One exception CO Lac, may be resolved if further spectroscopic observations lead to a 20 percent increase in the observed orbital velocities of the two components.

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