The birth rate of SNe Ia from hybrid CONe white dwarfs
Considering the uncertainties of the C-burning rate (CBR) and the treatment of convective boundaries, Chen et al. (2014) found that there is a regime where it is possible to form hybrid CONe white dwarfs (WDs), i.e. ONe WDs with carbon-rich cores. As these hybrid WDs can be as massive as 1.30 $M_{\o...
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| Format: | Journal article |
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2014
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| _version_ | 1797102487947182080 |
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| author | Meng, X Podsiadlowski, P |
| author_facet | Meng, X Podsiadlowski, P |
| author_sort | Meng, X |
| collection | OXFORD |
| description | Considering the uncertainties of the C-burning rate (CBR) and the treatment of convective boundaries, Chen et al. (2014) found that there is a regime where it is possible to form hybrid CONe white dwarfs (WDs), i.e. ONe WDs with carbon-rich cores. As these hybrid WDs can be as massive as 1.30 $M_{\odot}$, not much mass needs to be accreted for these objects to reach the Chandrasekhar limit and to explode as Type Ia supernovae (SNe Ia). We have investigated their contribution to the overall SN Ia birth rate and found that such SNe Ia tend to be relatively young with typical time delays between 0.1 and 1 Gyr, where some may be as young as 30 Myr. SNe Ia from hybrid CONe WDs may contribute several percent to all SNe Ia, depending on the common-envelope ejection efficiency and the CBR. We suggest that these SNe Ia may produce part of the 2002cx-like SN Ia class. |
| first_indexed | 2024-03-07T06:06:39Z |
| format | Journal article |
| id | oxford-uuid:ee143317-b546-495d-b313-1582ce88263c |
| institution | University of Oxford |
| last_indexed | 2024-03-07T06:06:39Z |
| publishDate | 2014 |
| record_format | dspace |
| spelling | oxford-uuid:ee143317-b546-495d-b313-1582ce88263c2022-03-27T11:29:58ZThe birth rate of SNe Ia from hybrid CONe white dwarfsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:ee143317-b546-495d-b313-1582ce88263cSymplectic Elements at Oxford2014Meng, XPodsiadlowski, PConsidering the uncertainties of the C-burning rate (CBR) and the treatment of convective boundaries, Chen et al. (2014) found that there is a regime where it is possible to form hybrid CONe white dwarfs (WDs), i.e. ONe WDs with carbon-rich cores. As these hybrid WDs can be as massive as 1.30 $M_{\odot}$, not much mass needs to be accreted for these objects to reach the Chandrasekhar limit and to explode as Type Ia supernovae (SNe Ia). We have investigated their contribution to the overall SN Ia birth rate and found that such SNe Ia tend to be relatively young with typical time delays between 0.1 and 1 Gyr, where some may be as young as 30 Myr. SNe Ia from hybrid CONe WDs may contribute several percent to all SNe Ia, depending on the common-envelope ejection efficiency and the CBR. We suggest that these SNe Ia may produce part of the 2002cx-like SN Ia class. |
| spellingShingle | Meng, X Podsiadlowski, P The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title | The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title_full | The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title_fullStr | The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title_full_unstemmed | The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title_short | The birth rate of SNe Ia from hybrid CONe white dwarfs |
| title_sort | birth rate of sne ia from hybrid cone white dwarfs |
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