Evolutionary Pathways Leading to Double Degenerate Mergers and SN Ia Progenitors

Astronomy and Astrophysics – Astronomy

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Scientific paper

It is still not clear what the progenitors of Type Ia Supernovae (SN Ia) are. There are currently two major competing (or compatible) formation channels under consideration: the single-degenerate scenario and the double-degenerate scenario (DDS). A DDS SN Ia is the result of the merger of two white dwarfs whose combined mass exceeds that of the Chandrasekhar mass. Even though the Milky Way disc alone is host to 108 double white dwarfs, such events are expected to be rare in our Galaxy ( 0.1/century), given the long timescales associated with gravitational wave emission which ultimately leads to double white dwarf mergers. Nonetheless, extragalactic observations of SN Ia lend strong support to the DDS channel. We aim to understand the processes in binary evolution which most favourably lead to the formation of SN Ia in the DDS. In our (population synthesis) evolutionary calculations, we take into account i.e.: star formation history, metallicity, common envelope evolution, and mass transfer phases. We will present the initial conditions which lead most favourably to the formation of SN Ia progenitors, show the associated rates and delay times (star formation to SN Ia), and comment on the most (and least) likely host environments for these systems.
AJR acknowledges the hospitality and financial support of the Radboud University Astronomy Dept.

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