Rare events of a peculiar thermonuclear supernova that precedes a core collapse supernova. (arXiv:2103.07884v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Bear_E/0/1/0/all/0/1">Ealeal Bear</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel)
We study stellar binary evolution that leads to the formation of a white
dwarf (WD) that explodes in a thermonuclear supernova at the termination of a
common envelope evolution (CEE) shortly before the core of its companion
explodes as a core-collapse supernova (CCSN). The CCSN explosion of the core,
which is the remnant of a red supergiant (RSG) star, might take place few
months to several years after the explosion of the WD as a thermonuclear
supernova, i.e., a type Ia peculiar supernova (peculiar SN Ia). Using the
evolutionary code MESA-binary we simulate evolution of binary systems with
stars of initial masses of 6-7.5Mo. The more massive star, the primary,
transfers mass to the secondary star and leaves a CO WD remnant. The secondary
becomes massive enough to end in a CCSN. As the secondary evolves to the RSG
phase it engulfs the WD and the system experience a CEE that ends with a
WD-core binary system at an orbital separation of a_f ~ 1-5Ro. Our simulations
show that the core explodes as a CCSN at t_{CEE-CCSN} ~ 3000 – 10^5 yr after
the CEE. We assume that if the WD accretes helium-rich gas from the core it
might explode as a SN Ia in the frame of the double detonation scenario for SNe
Ia and peculiar SNe Ia. We predict the very rare occurrence of a peculiar SN Ia
followed within months to years by a CCSN.
We study stellar binary evolution that leads to the formation of a white
dwarf (WD) that explodes in a thermonuclear supernova at the termination of a
common envelope evolution (CEE) shortly before the core of its companion
explodes as a core-collapse supernova (CCSN). The CCSN explosion of the core,
which is the remnant of a red supergiant (RSG) star, might take place few
months to several years after the explosion of the WD as a thermonuclear
supernova, i.e., a type Ia peculiar supernova (peculiar SN Ia). Using the
evolutionary code MESA-binary we simulate evolution of binary systems with
stars of initial masses of 6-7.5Mo. The more massive star, the primary,
transfers mass to the secondary star and leaves a CO WD remnant. The secondary
becomes massive enough to end in a CCSN. As the secondary evolves to the RSG
phase it engulfs the WD and the system experience a CEE that ends with a
WD-core binary system at an orbital separation of a_f ~ 1-5Ro. Our simulations
show that the core explodes as a CCSN at t_{CEE-CCSN} ~ 3000 – 10^5 yr after
the CEE. We assume that if the WD accretes helium-rich gas from the core it
might explode as a SN Ia in the frame of the double detonation scenario for SNe
Ia and peculiar SNe Ia. We predict the very rare occurrence of a peculiar SN Ia
followed within months to years by a CCSN.
http://arxiv.org/icons/sfx.gif
