Evolution Of Post-Impact Remnant Helium Stars In Type Ia Supernova Remnants Within The Single-Degenerate Scenario

Дата и время публикации : 2013-03-06T01:10:19Z

Авторы публикации и институты :
Kuo-Chuan Pan
Paul Ricker
Ronald Taam

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 37 pages, 12 figures, accepted for publication in ApJ
Первичная категория: astro-ph.HE

Все категории : astro-ph.HE, astro-ph.SR

Краткий обзор статьи: The progenitor systems of Type Ia supernovae (SNe Ia) are still under debate. Based on recent hydrodynamics simulations, non-degenerate companions in the single-degenerate scenario (SDS) should survive the supernova impact. One way to distinguish between the SDS and the double-degenerate scenario is to search for the post-impact remnant stars (PIRSs) in SN Ia remnants. Using a technique that combines multi-dimensional hydrodynamics simulations with one-dimensional stellar evolution simulations, we have examined the post-impact evolution of helium-rich binary companions in the SDS. It is found that these helium-rich PIRSs (He PIRSs) dramatically expand and evolve to a luminous phase ($Lsim 10^4 L_odot$) about 10 years after a supernova explosion. Subsequently, they contract and evolve to become hot blue-subdwarf-like (sdO-like) stars by releasing gravitational energy, persisting as sdO-like stars for several million years before evolving to the helium red-giant phase. We therefore predict that a luminous OB-like star should be detectable within $sim 30$ years after the SN explosion. Thereafter, it will shrink and become an sdO-like star in the central regions of SN Ia remnants within star-forming regions for SN Ia progenitors evolved via the helium-star channel in the SDS. These He PIRSs are predicted to be rapidly rotating ($v_{rm rot} gtrsim 50$ km s$^{-1}$) and to have high spatial velocities ($v_{rm linear} gtrsim 500$ km s$^{-1}$). Furthermore, if supernova remnants have diffused away and are not recognizable at a later stage, He PIRSs could be an additional source of single sdO stars and/or hypervelocity stars.

Category: Physics