Photometric study of the eclipsing binary WX Cephei

Details Photometric study of the eclipsing binary WX Cephei Photometric study of the eclipsing binary WX Cephei

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pasp...87..795e&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 87, Oct. 1975, p. 795-800.

Astronomy and Astrophysics

Astronomy

5

A Stars, Eclipsing Binary Stars, Stellar Spectrophotometry, Ubv Spectra, Electrophotometry, Light Curve, Orbital Elements, Stellar Luminosity, Stellar Mass, Stellar Temperature

Scientific paper

The photometric elements of the eclipsing binary WX Cep are determined from 3120 photoelectrically measured observations in each of the B and V regions which were obtained in the summer of 1973 at the Pine Mountain Observatory of the University of Oregon. The analysis shows that primary minimum is produced by the occultation of the smaller, fainter type A2 star by the larger brighter star of about type A5, and that during the 10.9-hour duration of the primary eclipse it is total for about 40 minutes. The existing spectroscopic data (of uncertain quality) for this double-line binary are used to estimate the mass and radius of each component. Both components have about one solar mass which is somewhat smaller than expected for these spectral classes even if the luminosity class of each star is V.

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