Volume 367, Number 1, February III 2001
|Page(s)||199 - 210|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2001|
A photometric and spectroscopic study of the eclipsing symbiotic binary AX Persei*
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia
2 Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
3 Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
Corresponding author: A. Skopal, firstname.lastname@example.org
Accepted: 7 November 2000
We analysed photometric and spectroscopic optical observations of the eclipsing symbiotic binary AX Persei. For the first time, we present and discuss its historical, 1887-1999, photographic/B-band and visual light curve (LC). The red giant in AX Per losses mass via the wind at a rate of . The terminal velocity of the wind is . We estimated an effective radius of the Hii nebula during the post-outburst stage (to JD 2450000) to be of and its average electron concentration for the electron temperature Te = 1-1.5 104 K. The [Oiii] nebula in AX Per is rather dense, having the electron concentration ne([Oiii]) for Te = 1-1.5 104 K. Spectroscopic observations made in the middle of the 1992.8 and 1994.7 eclipses showed that a significant part of flux emitted in the Hi, Heii and nebular [Oiii] lines originates in the vicinity of the hot component. Transition of AX Per to its nebular phase occurred at/around JD 2450000. A small ∼0.6 mag brightening at that time and consequently very broad wave-like variation in the LC developed. This event was caused by dilution of a shell around the hot star, during which about of 1.5 1050 particles (∼ ) were injected into the ionized region.
Key words: stars: binaries: symbiotics / stars: circumstellar matter / stars: mass-loss
© ESO, 2001
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