Apsidal motion and revised photometric elements of the eccentric eclipsing binary V 477 Cygni

Details Apsidal motion and revised photometric elements of the eccentric eclipsing binary V 477 Cygni Apsidal motion and revised photometric elements of the eccentric eclipsing binary V 477 Cygni

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...260..227g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 260, no. 1-2, p. 227-236.

Astronomy and Astrophysics

Astrophysics

24

Apsides, Eclipsing Binary Stars, Stellar Motions, Stellar Spectrophotometry, Eccentric Orbits, Stellar Magnitude

Scientific paper

The paper determines accurate physical parameters for the component stars of the eclipsing binary V 477 Cygni. A rediscussion of the photometric data of O'Connell (1970) using an extended version of the synthetic light curve computer code EBOP, which takes into account the variable position of the periastron, is carried out. The obtained results, combined with existing radial velocity curves by Popper (1968), lead to absolute radii of 1.57 +/- 0.05 (star A) and 1.27 +/- 0.04 (star B) and solar masses of 1.79 +/- 0.12 and 1.35 +/- 0.07. The orbit of V 477 Cygni is highly eccentric (e = 0.307), and an apsidal motion rate with a period of 350 +/- 10 yr is found. The internal structure constant derived from the observed apsidal motion rate (log k(2) = -2.20 +/- 0.04) indicates a slightly less centrally concentrated configuration than predicted by theoretical models.

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