A polarimetric study of U Cephei. I

Details A polarimetric study of U Cephei. I A polarimetric study of U Cephei. I

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90...48p&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 1-2, Oct. 1980, p. 48-53.

Astronomy and Astrophysics

Astrophysics

19

Astronomical Photometry, Cepheid Variables, Eclipsing Binary Stars, Polarimetry, Stellar Envelopes, Interstellar Matter, Light Curve, Optical Thickness, Roche Limit, Stellar Models

Scientific paper

Polarimetric observations of U Cephei in 1972-78 are presented. Time- and phase-dependent variations in polarization and changes in the shape of the light curve are discussed. The observations of the 1974-75 outburst cannot be explained by an optically thin envelope or disk surrounding the primary component. The observed polarization is an order of magnitude too small when compared with the amount of additional light during the totality of the primary eclipse. It is suggested that the effective radius of the photosphere of the primary is increased by 15-20% during the periods of high mass transfer. The polarization observations could then be explained by a simple model containing an optically thin spherical envelope of outer radius 1.1 times the primary photosphere effective radius and an equatorial disk of outer radius 1.7 times the primary photosphere effective radius surrounding the primary. The mean electron density is about 1.4 x 10 to the 12th/cu cm in the spherical envelope and 1.6 x 10 to the 12th/cu cm in the preceding and 0.9 x 10 to the 12th/cu cm in the trailing sides of the disk, the thickness of which is assumed to be 0.1 times the primary photosphere effective radius normal to the orbital plane. The variations in the position angle can be explained if the inclination of the orbit is about 83 deg.

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