Photometric Variability of HD 51585 (Arkhipova+, 2006)

Details Photometric Variability of HD 51585 (Arkhipova+, 2006) Photometric Variability of HD 51585 (Arkhipova+, 2006)

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ycat..90320662a&link_type=abstract

VizieR On-line Data Catalog: J/PAZh/32/662. Originally published in: 2006PAZh...32..662A; 2006AstL...32..594A

Astronomy and Astrophysics

Astronomy

Stars: Be, Spectroscopy, Photometry: Ubv

Scientific paper

Photoelectric observations of HD 51585 (OY Gem), a B[e] star with an infrared excess and a candidate for protoplanetary nebulae, obtained with a 60-cm telescope at the Crimean Station of the Sternberg Astronomical Institute in 1992-2005 are presented. The star exhibited rapid irregular brightness variations with amplitudes from 0.1mag in the V band to 0.2mag in the U band within the observing season as well as slow systematic variations with amplitudes from 0.3mag in the V band to 0.65mag in the U band and with a quasi-period of ~2800days. The B-V color index varied within 0.1mag and did not follow the slow systematic brightness variations, while U-B correlated with the U brightness and varied between 0.7mag at maximum light and 0.35mag at minimum light. Our low-resolution spectroscopy performed in 1994-2005 has revealed significant variability of the Balmer and Paschen hydrogen emission lines as well as the He I and OI lines. Equivalent widths are given for the HI, He I, OI, and Fe II lines; a correlation has been found between the star's photometric variability and the hydrogen line intensities. Our joint analysis of the photometric and spectroscopic data suggests that variations in a strong stellar wind are responsible for the variability of the star.
(1 data file).

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