Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae

Wu, Chenjie; Wang, Bo; Liu, D.; Han, Zhanwen

doi:10.1051/0004-6361/201630099

Cited by 35 publications

(42 citation statements)

References 58 publications

(81 reference statements)

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“…As well, masstransfer rates based on the latter M-R relation, excellently agree with those, based on M-R relation for finite, but low, entropy WDs suggested by Bildsten et al (2006). 1 We remind also that, as found first by Nomoto (1982) and, most lately, e.g., in our Paper I and by Brooks et al (2015); Wu et al (2017), He-burning may occur in the following regimes (in the order of increasing accretion rate M accr ).…”

Section: Introductionsupporting

confidence: 86%

He-accreting WD: nucleosynthesis in the extreme binary system (1.02 + 0.30) M⊙

Piersanti

Yungelson

Cristallo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the evolutionary properties of AM CVn stars with massive white dwarf donors and accretors. As a representative of them we consider a binary initially composed by a 0.30M ⊙ He WD and a 1.02M ⊙ CO WD. We evaluate the time-dependent mass transfer rate from the donor and compute the evolution of the accretor, accounting for the effects of mass exchange on the evolution of orbital parameters. We model the thermal response of the accreting CO WD with the FUN evolutionary code coupled to a full nuclear network, from H to Bi, including more than 700 isotopes linked by about 1000 nuclear processes. We find that accretors in these systems evolve through the stages of steady He-burning and mild and strong He-flashes and become at the end CO WDs capped by a massive (∼ 0.1M ⊙ ) He-rich buffer. During He-flashes (both mild and strong) the temperature in the He-shell increases above 3 × 10 8 K, so that the 22 Ne(α, n) 25 Mg reaction becomes efficient and n-rich isotopes can be produced. During the RLOF episodes triggered by strong non-dynamical He-flashes matter enriched in α-elements and n-rich isotopes is ejected, polluting the interstellar medium. Our results strongly suggest that massive AM CVn systems with WD donors do not experience a final very strong dynamical He-flash driving an explosive event like SN .Ia. Though the ejected matter is highly enriched in heavy isotopes, the relative contribution of massive AM CVn systems to the Galactic chemical evolution is, most probably, negligible due to their expected paucity.

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Section: Introductionsupporting

confidence: 86%

He-accreting WD: nucleosynthesis in the extreme binary system (1.02 + 0.30) M⊙

Piersanti

Yungelson

Cristallo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…We note in passing that He retention efficiencies have also been published by Piersanti et al (2014) and Wu et al (2017). As the former extend only up to a WD mass of ≈ 1 M , they cannot be applied in the evolution up to explosion.…”

Section: Mass Retention Efficiencymentioning

confidence: 91%

Inlists and Output files for paper: Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae

Wong,

Schwab,

Götberg

2021

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Helium star -carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code MESA, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to NUV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultramassive WD in a multi-day orbit. However, extending our binary models to initial CO WD masses of up to 1.2 M , we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star -WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition.

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“…Their calculated values of η He are generally between those of Kato & Hachisu (2004) and Wang et al (2015). Assuming that there are supper-Eddington winds during multi-cycle He-shell flashes, Wu et al (2017) also calculated the values of η He , and found them to be lower than those in Kato & Hachisu (2004).…”

Section: Non-magnetic Wdsmentioning

confidence: 95%

A Study of Magnetized White Dwarf + Helium Star Binary Evolution to Type Ia Supernovae

Cui,

2021

Preprint

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The white dwarf (WD) + helium (He) star binary channel plays an important role in the single degenerate scenario for the progenitors of type Ia supernovae (SNe Ia). Previous studies on the WD + main sequence star evolution have shown that the magnetic fields of WDs may significantly influence their accretion and nuclear burning processes. In this work we focus on the evolution of magnetized WD + He star binaries with detailed stellar evolution and binary population synthesis (BPS) calculations. In the case of magnetized WDs, the magnetic fields may disrupt the inner regions of the accretion disk, funnel the accretion flow onto the polar caps, and even confine helium burning within the caps. We find that, for WDs with sufficiently strong magnetic fields, the parameter space of the potential SN Ia progenitor systems shrinks toward shorter orbital periods and lower donor masses compared with that in the non-magnetized WD case. The reason is that the magnetic confinement usually works with relatively high mass transfer rates, which can trigger strong wind mass loss from the WD, thus limiting the He-rich mass accumulation efficiency. The surviving companion stars are likely of low-mass at the moment of the SN explosions, which can be regarded as a possible explanation for the non-detection of surviving companions after the SNe or inside the SN remnants.However, the corresponding birthrate of Galactic SNe Ia in our high-magnetic models is estimated to be ∼ (0.08 − 0.13) × 10 −3 yr −1 (∼ 0.17 − 0.28 × 10 −3 yr −1 for the non-magnetic models), significantly lower than the observed Galactic SN Ia birthrate.

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Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae

Cited by 35 publications

References 58 publications

He-accreting WD: nucleosynthesis in the extreme binary system (1.02 + 0.30) M⊙

He-accreting WD: nucleosynthesis in the extreme binary system (1.02 + 0.30) M⊙

Inlists and Output files for paper: Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae

A Study of Magnetized White Dwarf + Helium Star Binary Evolution to Type Ia Supernovae

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