Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000astl...26..233m&link_type=abstract
Astronomy Letters, vol. 26, p. 233-243 (2000)
Astronomy and Astrophysics
Astronomy
1
Scientific paper
The UBVR photometry of XY Per in 1985-1998 is presented. At this epoch, XY Per exhibited variability with an amplitude of approximately 1 mag in V. The photometric variability of XY Per can be divided into three components: (1) smooth year-to-year variations in mean brightness; (2) quasi-periodic variations with a characteristic time scale of 20-40 days and an amplitude of 0.3 mag; and (3) Algol-like minima with a duration of 15-20 days and an amplitude of 0.6 mag. The CLEAN algorithm is used to refine the quasi-period of light variations in the interval 1988-1995, P = 22.7252 days. The observed variability is assumed to be produced by two mechanisms: circumstellar absorption and nonstationary accretion. An ultraviolet excess was observed in the stellar radiation during the local minimum of 1991, which was associated with an eclipse of the star by a circumstellar formation. The probable reason why it emerged is that part of the eclipsing circumstellar formation fell into the accretion zone. A high-resolution spectrum in the wavelength range 3600-6700 A contains both photospheric lines and circumstellar shell lines. The shell line profiles suggest mass accretion onto the star at a velocity of 90-140 km/s. Of the Balmer lines, only H_alpha is in emission. Its equivalent width is E(W_lambda) = -0.8 A. The strongest FeII lines, as well as MgII 4481.33 A and HeI 5875.65 A, have an emission component at the line center. The presence of emission components in lines with different excitation potentials suggests the presence of a hot gas shell around the star, which is heated very nonuniformly.
Ezhkova O. V.
Melnikov Stanislav Yu.
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