RW Persei and the disk hypothesis

Details RW Persei and the disk hypothesis RW Persei and the disk hypothesis

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aj.....95.1828w&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 95, June 1988, p. 1828-1836. Research supported by the University of Florida and Uni

Astronomy and Astrophysics

Astronomy

16

Accretion Disks, Eclipsing Binary Stars, Light Curve, Stellar Rotation, Angular Velocity, Mass Ratios

Scientific paper

The Algol-type semidetached eclipsing binary system RW Persei is rediscussed, based on two new developments. The photometric light curve obtained by Hall and Stuhlinger (1978) has been rediscussed with explicit modeling of a circumstellar disk, as advocated for RW Persei by Hall. No compelling evidence was found for such a disk, but different parameters have been obtained, making RW Persei a much more ordinary Algol system. In the improved model, the primary star is a B9.6e IV-V main sequence star (slightly evolved) with mass 2.6 and radius 2.8 solar units, while the corresponding values for the K2 III-IV secondary are 0.4 and 7.3 solar units, respectively. The revised distance to the system is about 440 pc; its large color excess, E(B-V) = 0.40 mag, is mainly due to its low galactic latitude combined with this distance. There is photometric evidence for a third star which contributes about 8% of the total system light in V, and is about 0.2 - 0.3 mag redder in B-V than the system.

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