The white dwarf's carbon fraction as a secondary parameter of Type Ia supernovae
Methods. The explosion phase is simulated using the finite volume supernova code Leafs, which is extended to treat different compositions of the progenitor WD. The synthetic observables are computed with the Monte Carlo radiative transfer code Artis. Results. Differences in binding energies of carbon and oxygen lead to a lower nuclear energy release for carbon depleted material; thus, the burning fronts that develop are weaker and the total nuclear energy release is smaller. For otherwise...[Show more]
|Collections||ANU Research Publications|
|Source:||Astronomy and Astrophysics|
|Access Rights:||Open Access|
|01_Ohlmann_The_white_dwarf's_carbon_2014.pdf||1.49 MB||Adobe PDF|
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