Spectroscopic and photometric variability of HD 51585 as a manifestation of stellar wind

Details Spectroscopic and photometric variability of HD 51585 as a manifestation of stellar wind Spectroscopic and photometric variability of HD 51585 as a manifestation of stellar wind

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006astl...32..594a&link_type=abstract

Astronomy Letters, vol. 32, Issue 9, p.594-603

Astronomy and Astrophysics

Astronomy

Pacs Numbers 97.85.Eh

Scientific paper

We present the results of our 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. The star exhibited rapid irregular brightness variations with amplitudes from in the V band to in U band within the observing season as well as slow systematic variations with amplitudes from in the V band to in the U band and with a quasi-period of ˜2800 days. The B-V color index varied within &
$0(m) .1
; and did not follow the slow systematic brightness variations, while U-B correlated with the U brightness and varied between &
- 0(m) .7
; at maxiμm light and &
- 0(m) .35$
; 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 O I lines. Equivalent widths are given for the H I, He I, O I, 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.

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