CAOSP abstracts, Volume: 30, No.: 1, year: 2000
- Author(s): SKOPAL, A.; PRIBULLA, T.; WOLF, M.; SHUGAROV, S.Y.; JONES, A.
- Journal: Contributions of the Astronomical Observatory Skalnate Pleso,
vol. 30, no. 1, p. 29-42.
- Date: 04/2000
- Title: Photometry of symbiotic stars. IX. TX CVn, CH Cyg, AX Per and AR Pav
- Keyword(s): STARS, BINARIES, SYMBIOTICS, PHOTOMETRY
- Pages: 29 -- 42
We present new photometric observations of TX CVn, CH Cyg, AX Per and
AR Pav. The main results can be summarized as follows:
TX CVn: The historical 1893-2000 photographic/B-band light curve (LC) is
presented for the first time. From 1892 to ~1920, the star was quiet, but then
entered a series of outbursts peaking in 1920, 1945, 1952 and 1962. From ~1988
till the present time, TX Cvn has gradually declined.
CH Cyg: Our observations cover an active phase, which began in May 1998. At
the beginning of June 1999 the star's brightness in the U band rapidly
decreased due to an eclipse of the active inner binary (the symbiotic pair) by
a cool giant in the outer orbit.
AX Per: The historical 1887-2000 photographic/B-band LC is summarized here
for the first time. It is characterized by long-lasting periods of quiescence
with the superposition of a few bright stages lasting about 1.5 orbital cycles.
Our photoelectric U,B,V observations revealed a drastic change in the LC
profile, which occurred after JD 2 450 000 (1995.8). A small 0.6 mag flare at
that time and consequently very broad wave-like variation in the LC developed.
This event was caused by the dilution of a shell around the hot star.
AR Pav: Our observations show that the recent active phase, which began in
1985.7 is over. During the activity, AR Pav developed a complex wave-like
variation at the level of ~1.5 mag in the visual band. The transition to a
quiet phase was rapid -- the wave-like variation disappeared.
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