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A close look at the outburst of the very slow symbiotic nova PU Vul – a triple system

Published online by Cambridge University Press:  12 April 2016

D. Chochol ,
S. Tamura ,
O. Kanamitsu ,
T. Pribulla  and
A. Tajitsu
D. Chochol
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia
S. Tamura
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Aoba-ku, Sendai, Miyagi 980, Japan
O. Kanamitsu
Affiliation:
Fukuoka University of Education, 129 Akama, Munakata-shi, Fukuoka 811-41, Japan
T. Pribulla
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia
A. Tajitsu
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Aoba-ku, Sendai, Miyagi 980, Japan

Extract

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The very slow nova PU Vul was discovered by Honda and Kuwano in 1979 after the rise from B ~ 15…16 mag to a maximum B ~ 9 mag. The object has been studied by many authors (for references see Belyakina et al. 1989; Vogel & Nussbaumer 1992) but a clear picture of the system was not given. Two minima of different duration were observed in the system in the active stage, in 1980-81 and 1993-94 (Kolotilov et al. 1995). Nussbaumer & Vogel (1996) ascribed the minima to eclipses of the hot component by the cool M giant in a binary with orbital period of 4900±100 d. Our period analysis of the preoutburst B data (Liller & Liller 1979) by Stellingwerf’s (1978) method revealed a period of 4858 d. We found the third minimum in 1926-28 (lasting for 500…630 d) in these data.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 343 - 344
Copyright
Copyright © Kluwer 1996

References

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