The very short-period extreme mass ratio binary 75 Pegasi - Photometry and model

Details The very short-period extreme mass ratio binary 75 Pegasi - Photometry and model The very short-period extreme mass ratio binary 75 Pegasi - Photometry and model

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasp..103..424m&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 103, May 1991, p. 424-430. Research supported by NSERC,

Astronomy and Astrophysics

Astronomy

2

Astronomical Models, Eclipsing Binary Stars, Variable Stars, Astronomical Photometry, Limb Darkening, Stellar Luminosity

Scientific paper

The bright star 75 Peg is a close binary ellipsoidal variable with a
short period (0.5021035-day) and an extreme mass ratio of 0.104 B, V,
and R photometric data, along with previously published radial-velocity
data, are analyzed; they suggest that the primary of the 75 Peg system
may be, or is very close to, filling its critical Roche lobe.

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