CAOSP abstracts, Volume: 22, year: 1992
- Author(s): SKOPAL, A.; HRIC, L.; URBAN, Z.; PIGULSKI, A.; BLANCO, C.; PAPOUSEK, J.;
HANZL, D.; AGERER, F.; NIARCHOS, P.; ROVITHIS-LIVANIOU, H.; ROVITHIS, P.;
TSVETKOVA, K.; SEMKOV, E.; VELIC, Z.; MICHALEK, F.; KOMACKA, L.;
SCHWEITZER, E.; KORTH, S.
- Journal: Contributions of the Astronomical Observatory Skalnate Pleso,
vol. 22, p. 131-172.
- Date: 07/1992
- Title: Photometry of symbiotic stars - an international campaign. III. Z And,
EG And, R Aqr, UV Aur, TX CVn, T CrB, BF Cyg, CH Cyg, CI Cyg, V 1016 Cyg,
V 1329 Cyg, AG Dra, CQ Dra (4 Dra), YY Her, V 443 Her, SS Lep, RS Oph, AG Peg,
AX Per, HM Sge, FG Ser (AS 296), PU Vul
- Keyword(s): STARS, BINARIES, SYMBIOTIC, PHOTOMETRY
- Pages: 131 -- 172
Abstract:
We present new photoelectric (UBV), photographic and visual observations of
22 selected symbiotic stars. The photoelectric observations were made in
1990-91, the photographic in 1982-91, while the visual observations cover the
interval 1973-1991. Some interesting results can be summarized as follows:
EG And: Descending branches of the light-curve preceding primary and secondary
minima were observed in U. R Aqr: Visual observations confirm the variability
with the 44-year period. UV Aur: The 365-day pulsation period of the red giant
was confirmed. The most conspicuous change (7.2 - 10.4 mag) was observed in the
red band. BF Cyg: The eclipse of the hot component by the cool one was
observed between June and September 1991. Its position allowed to determine a
new average value of the orbital period equal to 759 days. CH Cyg: A sudden
drop of the star's brightness in U, by about 1.5 mag lasting a few days to a
few weeks was observed at the beginning of July 1991. 4 Dra: An 0.30 mag
increase in U, lasting about 100 days, was observed near the time of
spectroscopic conjunction. V 443 Her: A minimum around JD 2 448 433 was
observed in several spectral bands. AG Peg: A decrease of the star's
brightness near the orbital phase 0.5 was indicated. AX Per: The primary
minimum corresponding to the total eclipse of the hot component by the cool one
was observed between October 27, 1990 and January 14, 1991.
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