Helium Nova on a Very Massive White Dwarf: A Revised Light-Curve Model of V445 Puppis (2000)

• Published in: The Astrophysical journal Vol. 684; no. 2; pp. 1366 - 1373
• Main Authors: Kato, Mariko, Hachisu, Izumi, Kiyota, Seiichiro, Saio, Hideyuki
• Format: Journal Article
• Language: English
• Published: Chicago, IL IOP Publishing 10.09.2008; University of Chicago Press
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; stars: individual (V445 Puppis); White dwarf stars; Novae; Light curves; Mass loss; binaries: close; novae, cataclysmic variables; white dwarfs; Stellar mass; Close binary stars; Cataclysmic variable stars; Models; stars: mass loss
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/590329

V445 Pup (2000) is a unique object identified as a helium nova. Color indexes during the outburst are consistent with those of free-free emission. We present a free-free emission-dominated light-curve model of V445 Pup on the basis of the optically thick wind theory. Our light-curve fitting shows that (1) the white dwarf (WD) mass is very massive ([image] M sub([image])) and (2) half of the accreted matter remains on the WD, both of which suggest that the WD mass is increasing. Therefore, V445 Pup is a strong candidate for a Type Ia supernova progenitor. The estimated distance to V445 Pup is now consistent with recent observational suggestions, [image] kpc. A helium star companion is consistent with the brightness of [image] mag just before the outburst, if it is a slightly evolved hot star with the mass of [image] M sub([image]). We then emphasize importance of observations in the near- future quiescent phase after the thick circumstellar dust dissipates away, especially its color and magnitude, to specify the nature of the companion star. We have also calculated helium ignition masses for helium shell flashes against various helium accretion rates and discussed the recurrence period of helium novae.