2014MNRAS.438.3456P -
Mon. Not. R. Astron. Soc., 438, 3456-3464 (2014/March-2)
Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios.
PIRO A.L., THOMPSON T.A. and KOCHANEK C.S.
Abstract (from CDS):
We combine the observed distribution of Type Ia supernova (SN Ia) 56Ni yields with the results of sub-Chandrasekhar detonation and direct collision calculations to estimate what mass white dwarfs (WDs) should be exploding for each scenario. For collisions, the average exploding WD mass must be peaked at ~0.75M☉, significantly higher than the average field WD mass of ~0.55-0.60M☉. Thus, if collisions produce most SNe Ia, then a mechanism must exist that favours higher mass WDs. On the other hand, in old stellar populations, collisions would naturally result in low-luminosity SNe Ia, and we suggest these may be related to 1991bg-like events. For sub-Chandrasekhar detonations, the average exploding WD mass must be peaked at ~1.1M☉. This is similar to the average total mass in WD-WD binaries, but it is not clear whether double degenerate mergers would synthesize sufficient 56Ni to match observed yields. If not, then actual ~1.1M☉ WDs would be needed for sub-Chandrasekhar detonations. Since such high-mass WDs are produced relatively quickly in comparison to the age of SN Ia environments, this would require either accretion on to lower mass WDs prior to ignition or a long time-scale between formation of the ~1.1M☉ WD and ignition.
Abstract Copyright:
© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)
Journal keyword(s):
nuclear reactions, nucleosynthesis, abundances - supernovae: general - white dwarfs
Simbad objects:
1
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