Common envelope to explosion delay time of type Ia supernovae. (arXiv:1905.06025v1 [astro-ph.HE])

Common envelope to explosion delay time of type Ia supernovae. (arXiv:1905.06025v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel)

I study the rate of type Ia supernovae (SNe Ia) within about a million years
after the assumed common envelope evolution (CEE) that forms the progenitors of
these SNe Ia, and find that the population of SNe Ia with short CEE to
explosion delay (CEED) time is few times 0.1 of all SNe Ia. I also claim for an
expression for the rate of these SNe Ia that occur at short times after the
CEE, t<10^6 yr, that is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED times are different (at least to some extend) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so called SNe Ia-CSM, and the rate of SNe Ia that on a time scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core degenerate (CD) scenario, to the double degenerate (DD) scenario, and to the double detonation (DDet) scenario with white dwarf companions.

I study the rate of type Ia supernovae (SNe Ia) within about a million years
after the assumed common envelope evolution (CEE) that forms the progenitors of
these SNe Ia, and find that the population of SNe Ia with short CEE to
explosion delay (CEED) time is few times 0.1 of all SNe Ia. I also claim for an
expression for the rate of these SNe Ia that occur at short times after the
CEE, t<10^6 yr, that is different from that of the delay time distribution
(DTD) billions of years after star formation. This tentatively hints that the
physical processes that determine the short CEED times are different (at least
to some extend) from those that determine the DTD at billions of years. To
reach these conclusions I examine SNe Ia that interact with a circumstellar
matter (CSM) within months after explosion, so called SNe Ia-CSM, and the rate
of SNe Ia that on a time scale of tens to hundreds of years interact with a CSM
that might have been a planetary nebula, so called SNe Ia inside a planetary
nebula (SNIPs). I assume that the CSM in these populations results from a CEE,
and hence this study is relevant mainly to the core degenerate (CD) scenario,
to the double degenerate (DD) scenario, and to the double detonation (DDet)
scenario with white dwarf companions.

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