A Light-Curve Model of the Symbiotic Nova PU Vul (1979) -- A Very Quiet Explosion with Long-Lasted Flat Peak

Abstract

We present a light curve model of the symbiotic nova PU Vul (Nova Vulpeculae 1979) that shows a long-lasted 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 ~0.6 Mo. 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.

10 pages, 7 figures, published in ApJ, 2011, 727, 72

References in corpus (5)

• A Universal Decline Law of Classical Novae
• Broad H-alpha wings from the optically thin stellar wind of the hot components in symbiotic binaries
• A Universal Decline Law of Classical Novae. III. GQ Mus 1983
• Multiplicity of Nova Envelope Solutions and Occurrence of Optically Thick Winds
• Modeling of the Super-Eddington Phase for Classical Novae: Five IUE Novae

Cited by in corpus (9)

• The UBV Color Evolution of Classical Novae. I. Nova-Giant Sequence in the Color-Color Diagram
• A Light Curve Analysis of Classical Novae: Free-free Emission vs. Photospheric Emission
• Effects of a Companion Star on Slow Nova Outbursts -- Transition from Static to Wind Evolutions
• Evolution of the Symbiotic Nova PU Vul -- Outbursting White Dwarf, Nebulae, and Pulsating Red Giant Companion
• Novae in Globular Clusters
• DASCH Discovery of A Possible Nova-like Outburst in A Peculiar Symbiotic Binary
• An X-Ray and Optical Light Curv Model of the Eclipsing Symbiotic Binary SMC3
• ASASSN-16oh: A nova outburst with no mass ejection -- A new type of supersoft X-ray source in old populations
• Theoretical light curve models of the symbiotic nova CN Cha -- Optical flat peak for three years