Masses and radii for thirteen chromospherically active ellipsoidal variables

Details Masses and radii for thirteen chromospherically active ellipsoidal variables Masses and radii for thirteen chromospherically active ellipsoidal variables

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100..554h&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 100, Aug. 1990, p. 554-558.

Astronomy and Astrophysics

Astronomy

35

Chromosphere, Eclipsing Binary Stars, Stellar Atmospheres, Stellar Mass, Variable Stars, Main Sequence Stars, Roche Limit, Stellar Luminosity, Stellar Rotation

Scientific paper

The amplitude of the ellipticity effect, the mass function, and the V sin i in ten long-period RS CVn SB1 binaries are used to compute limits on the masses of the two stars and the radius of the primary: zeta And, UV CrB, V1764 Cyg, V826 Her, V350 Lac, GX Lib, V1197 Ori, AP Psc, 33 Psc, and EE UMa. Explicit masses and radii are computed for three SB2 systems: BL CVn, V1817 Cyg, and TZ Tri. The primary in several is found to fill 95 percent or more of its Roche lobe. The two minima produced by the ellipticity effect are unequal in depth, with the effect largest when i is near 90 deg and the primary nearly fills its Roche lobe. The greatest inequality found, in UV CrB, was 0.08 mag.

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