A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

Meng, Xiangcun; Podsiadlowski, Ph.

doi:10.1093/mnras/stx1137

Cited by 55 publications

(125 citation statements)

References 183 publications

(263 reference statements)

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“…Recently, Meng & Podsiadlowski (2017) developed a new version of the SD model, i.e. the commonenvelope wind (CEW) model which is completely different from the optically thick wind (OTW) model in physics (Hachisu et al 1996).…”

Section: Methodsmentioning

confidence: 99%

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

Meng

2018

Monthly Notices of the Royal Astronomical Society

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Although type Ia supernovae (SNe Ia) are so important in many astrophysical fields, a debate on their progenitor model is still endless. Searching the surviving companion in a supernova remnant (SNR) may distinguish different progenitor models, since a companion still exists in the remnant for the single-degenerate (SD) model, but does not for the double degenerate (DD) model. However, some recent surveys do not discover the surviving companions in the remnant of SN 1006 and Kepler's supernova, which seems to disfavor the SD model. Such a result could be derived from an incorrect survey target. Here, based on the common-envelope wind SD model for SNe Ia, in which the initial binary system consists of a white dwarf (WD) and a main-sequence (MS) star, we found that the companion at the moment of supernova explosion may be a MS, red-giant (RG) or subdwarf B (sdB) star if a spin-down timescale of less than 10 7 yr is assumed. We show the properties of the companions at the moment of supernova explosion, which are key clues to search the surviving companions in SNRs. Here, we suggest that the sdB star may be the surviving companion in some SNRs, even if the progenitor systems are the WD + MS systems. The SNe Ia with the sdB companions may contribute to all SNe Ia as much as 22%.

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Section: Methodsmentioning

confidence: 99%

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

Meng

2018

Monthly Notices of the Royal Astronomical Society

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“…In the CD scenario the CEE forms the single WD merger product of the core and the WD companion. In the CEE-wind channel of the SD scenario the CEE ensures the right conditions to bring the WD to explode (Meng, & Podsiadlowski 2017). These suggest that an important time of evolution is the time from the end of the CEE to the explosion itself, i.e., t CEED .…”

Section: Common Envelope To Explosion Delay (Ceed) Timementioning

confidence: 99%

“…If the explosion takes place after a long delay, it might leave behind a subdwarf B star or a WD. In the CEE-wind SD scenario that Meng, & Podsiadlowski (2017) suggested, the explosion might occur shortly after a CEE if the WD is a hybrid CONe WD (Meng, & Podsiadlowski 2018). In this scenario, that Meng, & Podsiadlowski (2018) predict to be ≈ 5 − 10% of all SNe Ia, the WD accretes hydrogenrich material from the envelope of a giant star while it spirals-in and ejects the envelope.…”

Section: Introductionmentioning

confidence: 99%

Common envelope to explosion delay time of Type Ia supernovae

Soker

2019

Monthly Notices of the Royal Astronomical Society

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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 × 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 CEED 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, to the double detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single degenerate (SD) scenario.

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“…Meng & Podsiadlowski (2018) even suggested that these two peculiar subclasses of SNe Ia share the same origin, i.e. from the hybrid CONe WD + MS system, based on a new developed version of singedegenerate model [common-envelope wind (CEW) model, Meng & Podsiadlowski 2017]. However, the CaII IR3 absorption features in the spectra of these peculiar SNe Ia are quite different from the normal SNe Ia.…”

Section: De and Ie Scenariosmentioning

confidence: 99%

“…the more massive the companion, the more likely to form a dense CSM by a wind (e.g. the commonenvelope wind, Meng & Podsiadlowski 2017). In addition, the age of an SN Ia from the SD channel is also dominated by the companion mass, i.e.…”

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confidence: 99%

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

Meng

2019

ApJ

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Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact nature is still unclear, e.g. the progenitor and explosion models. The high-velocity features (HVFs) in optical spectra of SNe Ia could provide some meaningful information to constrain the nature of SNe Ia. Here, I show strong evidence that the SNe Ia with strong CaII infrared triple (CaII IR3) HVF around maximum brightness associate with relatively younger population than those with weak CaII IR3 HVF, e.g. the SNe Ia with strong CaII IR3 HVF tend to occur in late-type galaxy, or early-type galaxy with significant star formation. In addition, using pixel statistics I find that the SNe Ia with strong maximum-light CaII IR3 HVF show a higher degree of association with star formation index, e.g. Hα or near-UV emission, than those with weak CaII IR3 HVF. Moreover, I find that the strength of the CaII IR3 HVF is linearly dependent on the difference of the absorption-weighted velocities between CaII IR3 and SiII 635.5 nm absorption lines, which then is a good index to diagnose whether or not there is a high-velocity component in the CaII IR3 absorption feature in the spectra of SNe Ia. I finally discussed the origin of the HVFs and the constraints from our discoveries on the progenitor model of SNe Ia.

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A common-envelope wind model for Type Ia supernovae – I. Binary evolution and birth rate

Cited by 55 publications

References 183 publications

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

Common envelope to explosion delay time of Type Ia supernovae

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

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