The ellipsoidal variable 42 Persei - Observations and model

Details The ellipsoidal variable 42 Persei - Observations and model The ellipsoidal variable 42 Persei - Observations and model

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasp..102.1153m&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 102, Oct. 1990, p. 1153-1160. Research supported by Kin

Astronomy and Astrophysics

Astronomy

2

Eclipsing Binary Stars, Stellar Models, Stellar Structure, Variable Stars, M Stars, Radial Velocity, Stellar Evolution, Stellar Luminosity, Stellar Spectrophotometry, Ubv Spectra

Scientific paper

The bright star 42 Per is an ellipsoidal variable with a period of 1.76535 days. New U, B, and V photometric data and radial velocities are analyzed in combination with previously published data. The model presented is a detached system with a mass ratio of approximately 0.19. If observed, a predicted shallow eclipse could contribute to a more reliable determination of the physical properties of the suspected M-type secondary star and the evolutionary state of the entire system.

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