Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..330..311k&link_type=abstract
The Astrophysics of Cataclysmic Variables and Related Objects, Proceedings of ASP Conference Vol. 330. Edited by J.-M. Hameury a
Astronomy and Astrophysics
Astrophysics
1
Scientific paper
The 2001 outburst of V445 Puppis shows unique properties, such as absence of hydrogen, enrichment of helium and carbon, slow light curve with a small amplitude that does not resemble to any type of novae. This object is suggested to be the first example of helium nova, and I have calculated theoretical light curves of helium novae and reproduce the observational light curve of V445 Pup. Fitting indicates a very massive white dwarf (> 1.3 M&sun;), with estimated ignition mass 5 × 10-5 {M&sun;}, which correspond to the helium accretion rate of 7 × 10-7 {M&sun;} yr-1 and the recurrence period of 70 years (for M=1.33 {M&sun;}). These values suggests that the white dwarf (WD) is growing in mass and ends up either a Type Ia supernova or an accretion induced collapse to form a neutron star. I have also calculated the mass accumulation efficiency during helium shell flashes for various white dwarf masses and the helium accretion rates. This efficiency is a crucial factor for binary evolutions to Type Ia supernovae. The efficiency takes the minimum values in between 1.1 and 1.2 {M&sun;} WD and increases in both less and more massive WDs. The mass accumulation efficiency is larger than 0.5 for log dM/dt(He) > -6.72 in all the WD masses.
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