Photometry of long-period algols. V - Multicolor solutions for RW Persei

Details Photometry of long-period algols. V - Multicolor solutions for RW Persei Photometry of long-period algols. V - Multicolor solutions for RW Persei

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....97..505o&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 97, Feb. 1989, p. 505-509.

Other

7

Accretion Disks, Eclipsing Binary Stars, Stellar Spectrophotometry, Ubv Spectra, Cool Stars, Optical Thickness, Stellar Rotation, Ultraviolet Spectra

Scientific paper

Photometric solutions are obtained for new uvbyI observations of RW Persei. In agreement with the conclusions of Wilson and Plavec (1988), these solutions require the hot gainer to rotate at close to 30 times its synchronous rate, in which state that star just fails to fill its rotational lobe. In the ultraviolet observations, shallow dips before and after primary eclipse may be the result of partial eclipses of a faint, optically thin accretion disk by the cool star. Otherwise, there is no evidence from continuum observations of a disk in this system. The effects of varying the rotational parameter F1 are demonstrated in light curves of primary eclipse.

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