TY - JOUR
T1 - Helium nova on a very massive white dwarf
T2 - A revised light-curve model of V445 Puppis (2000)
AU - Kato, Mariko
AU - Hachisu, Izumi
AU - Kiyota, Seiichiro
AU - Saio, Hideyuki
N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2008/9/10
Y1 - 2008/9/10
N2 - 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 (MWD ≳ 1.35 M ⊙) 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, 3.5 kpc ≲d≲6.5 kpc. A helium star companion is consistent with the brightness of mv = 14.5 mag just before the outburst, if it is a slightly evolved hot ( log T[K] ≳ 4.5) star with the mass of MHe ≳ 0.8 M⊙. 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.
AB - 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 (MWD ≳ 1.35 M ⊙) 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, 3.5 kpc ≲d≲6.5 kpc. A helium star companion is consistent with the brightness of mv = 14.5 mag just before the outburst, if it is a slightly evolved hot ( log T[K] ≳ 4.5) star with the mass of MHe ≳ 0.8 M⊙. 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.
KW - Binaries: close
KW - Novae, cataclysmic variables
KW - Stars: individual (V445 Puppis)
KW - Stars: mass loss
KW - White dwarfs
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U2 - 10.1086/590329
DO - 10.1086/590329
M3 - Article
AN - SCOPUS:52049086685
VL - 684
SP - 1366
EP - 1373
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
ER -