Single Degenerate Models for Type Ia Supernovae Progenitor's Evolution and Nucleosythesis Yields

Ken'ichi Nomoto; Shing-Chi Leung

doi:10.1007/s11214-018-0499-0

paper

Single Degenerate Models for Type Ia Supernovae Progenitor's Evolution and Nucleosythesis Yields

arXiv:1805.10811 · doi:10.1007/s11214-018-0499-0

Abstract

( $A b r i d g e d v er s i o n$ ) We review how the single degenerate models for Type Ia supernovae (SNe Ia) works. In the binary star system of a white dwarf (WD) and its non-degenerate companion star, the WD accretes either H-rich matter or He and undergoes H and He shell-burning. We summarize how such shell-burning depend on the accretion rate and the WD mass and how the WD blows strong wind. We identify the following evolutionary routes for the accreting WD to trigger a thermonuclear explosion. With a decreasing rate with time, 5 phases are observed: 1. The WD increases its mass by stable H burning and blows a strong wind, which strips a part of the companion star's envelope to control the accretion rate and forms circumstellar matter (CSM). The WD may explode within CSM as an "SN Ia-CSM". 2. The wind stops and an SN Ia is triggered under steady-stable H shell-burning, which is observed as a super-soft X-ray source: "SN Ia-SSXS". 3. H shell-burning becomes unstable and many flashes recur. The WD undergoes recurrent nova (RN) whose mass ejection is smaller than the accreted matter, evolving to an "SN Ia-RN". 4. If the companion is a He star or WD, the accretion of He can trigger He and C double detonations at the sub-Chandrasekhar (sub-Chand) mass or the WD grows to the Chand mass while producing and He-wind: "SN Ia-He CSM". 5. If the accreting WD rotates rapidly, delayed trigger of an SN Ia beyond standard Chand mass can happen. The (super-Chand) WD contracts to become a delayed SN Ia after losing angular momentum. The companion star has become a He WD and CSM has disappeared: "SN Ia-He WD". We update nucleosynthesis yields of the carbon deflagration model W7, delayed detonation model WDD2, and the sub-Chand mass model to constrain the yields (such as Mn) by comparing the observations. We note the important metallicity effects on $^{58}$ Ni and $^{55}$ Mn.

arXiv comment34 pages, 22 figures. Received at 8 March 2018 and accepted at 28 March 2018. Figures and tables updated to conform with other works in the series. Tables magnified for better vision

Single Degenerate Models for Type Ia Supernovae Progenitor's Evolution and Nucleosythesis Yields

Abstract

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