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| Paper: |
Repeating Novae and SNIa |
| Volume: |
490, Stella Novae: Past and Future Decades |
| Page: |
379 |
| Authors: |
Wallerstein, G. |
| Abstract: |
The repeating novae, stars such as T CrB, RS Oph, and a total of about 10 additional objects, have shown at least 2 outbursts. Only 5 (if you include V407 Cyg) show orbital periods greater than 200 days and consist of a white dwarf and a red giant. The other stars show orbital periods of less than 2 days. Several, including the bright stars T CrB and RS Oph, have shown coronal lines such as [Fe x] and [Fe XIV] during their outbursts. Probably more important is the derived mass of the white dwarf because in each long period system it is only slightly below the upper mass limit for a stable degenerate star. Mass transfer from the red giant is adding mass to the white dwarf that can be accumulated despite the loss during outbursts. Hence, the white dwarf may collapse and produce a supernova of type Ia. This type of single degenerate collapse may compete with the hypothesized double degenerate model as the origin of type Ia supernovae. |
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