Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237..496o&link_type=abstract
Astrophysical Journal, Part 1, vol. 237, Apr. 15, 1980, p. 496-505. NSF-supported research.
Astronomy and Astrophysics
Astrophysics
24
Eclipsing Binary Stars, Stellar Luminosity, Stellar Mass Accretion, B Stars, Disks (Shapes), Hot Stars, Mass Transfer, Optical Thickness
Scientific paper
Conspicuous excess light was seen between second and third contacts of primary eclipses in U Cep from late 1974 to late 1977. Part of this light was associated with a brightening of the outer hemisphere of the subgiant star, but most originated in optically thick accretion disks surrounding the hot B-type component. Disk light varied in times as short as 10 days. At peak size, outer disk radii were about 1.5R(B), and total vertical disk thicknesses were over half that of the B star. Various estimates of the mean mass-transfer rate in this 3 year interval suggest that the transfer rate was normal or slightly below normal, in spite of the observed disk activity.
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