Other
Scientific paper
Aug 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99r.142n&link_type=abstract
Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.142
Other
Scientific paper
There has been considerable debate over the true nature of the progenitors of Type Ia supernovae (SNe). Two of the most favoured binary models assume that the progenitor donor is either a degenerate dwarf that transfers matter onto another white dwarf (DD + CO), or that the donor is a main-sequence or red-giant branch star that loses matter to a white dwarf (MS + CO). For both cases it is assumed that the transferred matter burns in a quasi-steady state on the surface of the white dwarf thus allowing it to increase in mass. Assuming that the mass of the CO WD eventually exceeds the Chandrasekhar limit, a Type Ia SN ensues. The problem with both scenarios is that the synthetically inferred number of events does not match the observed frequency of Type Ia SNe. We have calculated a large number of evolutionary tracks to determine which systems can succeed in producing Type Ia SNe. It is shown that many more systems than previously thought can survive the initial mass-transfer phase and thereby allow the CO WD to accrete sufficient matter. We also examine the behaviour of the accreting COs in these binaries and show that many can remain smaller than their Roche-lobe radii during phases of thermal instability (hence avoiding the merger of the binary). We are presently carrying out a population synthesis to determine if enough progenitor systems can survive so as to match the inferred frequency of Type Ia events
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