A LIGHT-CURVE MODEL OF THE SYMBIOTIC NOVA PU Vul (1979): A VERY QUIET EXPLOSION WITH LONG-LASTING FLAT PEAK

Journal Article · Tue Feb 01 00:00:00 EST 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/727/2/72· OSTI ID:21567580

Kato, Mariko ^[1]; Hachisu, Izumi ^[2]; Cassatella, Angelo ^[3]; Gonzalez-Riestra, Rosario ^[4]

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1. Department of Astronomy, Keio University, Hiyoshi, Yokohama 223-8521 (Japan)
2. Department of Earth Science and Astronomy, College of Arts and Sciences, University of Tokyo, Komaba, Meguro-ku, Tokyo 153-8902 (Japan)
3. INAF, Istituto di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere 100, 00133 Roma (Italy)
4. XMM Sciece Operation Centre, ESAC, P.O. Box 78, 28091 Vallanueva de la Canada, Madrid (Spain)

We present a light-curve model of the symbiotic nova PU Vul (Nova Vulpeculae 1979) that shows a long-lasting flat peak with no spectral indication of wind mass loss before decline. Our quasi-evolution models consisting of a series of static solutions explain both the optical flat peak and ultraviolet (UV) light curve simultaneously. The white dwarf mass is estimated to be {approx}0.6 M{sub sun}. We also provide a new determination of the reddening, E(B - V) = 0.43 {+-} 0.05, from UV spectral analysis. Theoretical light-curve fitting of UV 1455 A provides the distance of d = 3.8 {+-} 0.7 kpc.

• OSTI ID: 21567580
• Journal Information: Astrophysical Journal, Vol. 727, Issue 2; Other Information: DOI: 10.1088/0004-637X/727/2/72; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
LOSSES
MASS
NOVAE
PEAKS
STELLAR WINDS
ULTRAVIOLET RADIATION
WHITE DWARF STARS
BINARY STARS
DWARF STARS
ELECTROMAGNETIC RADIATION
ERUPTIVE VARIABLE STARS
RADIATIONS
STARS
STELLAR ACTIVITY
VARIABLE STARS