An alternative symbiotic channel to Type Ia supernovae

Lü, Guo-Liang; Zhu, Chengliang; Wang, Zhaojun; Wang, Na

doi:10.1111/j.1365-2966.2009.14777.x

Cited by 76 publications

(87 citation statements)

References 77 publications

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“…Lü et al 2009;Toonen et al 2012;Meng & Yang 2012;Bours, Toonen & Nelemans 2013). In this study, however, we calculate the long-term evolution of the He-accreting CO WDs by solving their structure equations.…”

Section: Introductionmentioning

confidence: 99%

He-accreting carbon–oxygen white dwarfs and Type Ia supernovae

Wang

Podsiadlowski

Han

2017

Monthly Notices of the Royal Astronomical Society

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He accretion onto carbon-oxygen white dwarfs (CO WDs) plays a fundamental role when studying the formation of type Ia supernovae (SNe Ia). Employing the MESA stellar evolution code, we calculated the long-term evolution of Heaccreting CO WDs. Previous studies usually supposed that a WD can grow in mass to the Chandrasekhar limit in the stable He burning region and finally produce a SN Ia. However, in this study we find that off-centre carbon ignition occurs in the stable He burning region if the accretion rate is above a critical value (∼2.05 × 10 −6 M ⊙ yr −1 ), resulting in accretion-induced collapse rather than a SN Ia. If the accretion rate is below the critical value, explosive carbon ignition will eventually happen in the centre producing a SN Ia. Taking into account the possibility of off-centre carbon ignition, we have re-determined the initial parameter space that produces SNe Ia in the He star donor channel, one of the promising channels to produce SNe Ia in young populations. Since this parameter space is smaller than was found in the previous study of Wang et al. (2009), the SN Ia rates are also correspondingly smaller. We also determined the chemical abundance profile of the He-accreting WDs at the moment of explosive carbon ignition, which can be used as initial input for SN Ia explosion models.

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Section: Introductionmentioning

confidence: 99%

He-accreting carbon–oxygen white dwarfs and Type Ia supernovae

Wang

Podsiadlowski

Han

2017

Monthly Notices of the Royal Astronomical Society

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“…Over the past decade, many groups have widely investigated the single-degenerate model, in which the CO WD accretes H/He-rich material from a non-degenerate companion star. In this scenario, the donor star of WD may be a mainsequence star, a subgiant star or a red-giant star (see Hachisu et al 1996;Li & van den Heuvel 1997;Hachisu et al 1999a,b;Langer et al 2000;Han & Podsiadlowski 2004Chen & Li 2007;Chen & Li 2009;Meng et al 2009;Lü et al 2009;Wang et al 2010;Meng & Yang 2010a,b). Limongi & Tornambe (1991) were the first to study the evolution of the binary consisting of a CO WD and a He star, in which the CO WD accretes He matter from the He star and gains mass up to the canonical Chandrasekhar limit of 1.4 M .…”

Section: Introductionmentioning

confidence: 99%

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Liu

Chen

Wang

et al. 2010

A&A

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The recent discovery of several overluminous type Ia supernovae (SNe Ia) indicates that the explosive masses of white dwarfs may significantly exceed the canonical Chandrasekhar-mass limit. Rapid differential rotation may support these massive white dwarfs (WDs). Based on the single-degenerate scenario and assuming that the WDs would differentially rotate when the accretion ratė M > 3 × 10 −7 M yr −1 , we performed the numerical calculations for ∼1000 binary systems consisting of a He star and a CO WD with Eggleton's stellar evolution code. We present the initial parameters in the orbital period − helium star-mass plane (for WD masses of 1.0 M and 1.2 M , respectively), which lead to super-Chandrasekhar mass SNe Ia. Our results indicate that for an initially massive WD of 1.2 M , a large number of SNe Ia may result from super-Chandrasekhar mass WDs. The highest mass of the WD at the moment of the SNe Ia explosion is 1.81 M , but very massive (>1.85 M ) WDs cannot be formed. However, when the initial mass of WDs is 1.0 M , the explosive masses of SNe Ia are nearly uniform, which is consistent with the rareness of super-Chandrasekhar mass SNe Ia in observations.

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“…that a SN Ia originates from a CO WD in a binary system and that its companion is a main sequence or a slightly evolved star (WD+MS), a red giant star (WD+RG) or a helium star (WD + He star) (Whelan & Iben 1973;Nomoto et al 1984). This scenario has been widely studied by many groups (Li & van den Heuvel 1997;Hachisu et al 1999a;Langer et al 2000;Han & Podsiadlowski 2004;Chen & Li 2007;Hachisu et al 2008;Meng et al 2009;Lü et al 2009;Wang et al 2009a,b;Meng & Yang 2010b,c;Wang et al 2010). We assume that an initial CO WD is derived from a main sequence (MS) star in a primordial binary system (primary).…”

Section: Methodsmentioning

confidence: 99%

The correlation between C/O ratio, metallicity, and the initial WD mass for SNe Ia

Meng

Yang

2011

A&A

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Context. When type Ia supernovae (SNe Ia) were chosen as distance indicators to measure cosmological parameters, the Phillips relation was applied. However, the origin of the scatter in the maximum luminosity of SNe Ia (or the variation in the production of 56 Ni) remains unclear. Both the metallicity in general and the carbon abundance of a white dwarf (WD) before a supernova explosion are important parameters, but neither has the ability to interpret the scatter in the maximum luminosity of SNe Ia. Aims. We attempt to check whether or not the carbon abundance can be affected by initial metallicity. Methods. We calculated a series of stellar evolution models with various masses and metallicities. Results. We found that when Z ≤ 0.02, the carbon abundance is almost independent of metallicity if it is plotted against the initial WD mass. However, when Z > 0.02, the carbon abundance is not only a function of the initial WD mass, but also metallicity, i.e. for a given initial WD mass, the higher the metallicity, the lower the carbon abundance. On the basis of some previous studies, i.e. which find that both a high metallicity and a low carbon abundance lead to a lower production of 56 Ni being formed during a SN Ia explosion, the effects of the carbon abundance and the metallicity on the amount of 56 Ni are enhanced by each other, which may account, at least qualitatively, for the variation in the maximum luminosity of SNe Ia. Conclusions. Since the central density of WD before a supernova explosion may also play a role in the production of 56 Ni and the parameters (the carbon abundance, the metallicity, and the central density) are all determined by the initial parameters of the progenitor system, i.e. the initial WD mass, metallicity, orbital period and secondary mass, the amount of 56 Ni might be a function of the initial parameters. Then, our results might construct a bridge linking the progenitor model to the explosion model of SNe Ia.

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An alternative symbiotic channel to Type Ia supernovae

Cited by 76 publications

References 77 publications

He-accreting carbon–oxygen white dwarfs and Type Ia supernovae

He-accreting carbon–oxygen white dwarfs and Type Ia supernovae

Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

The correlation between C/O ratio, metallicity, and the initial WD mass for SNe Ia

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