A single-degenerate channel for the progenitors of Type Ia supernovae with different metallicities

Meng, Xiang-Cun; XF, Chen; Han, Zhanwen

doi:10.1111/j.1365-2966.2009.14636.x

Cited by 96 publications

(138 citation statements)

References 123 publications

(211 reference statements)

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“…Based on the comprehensive model, Meng & Yang (2010b) derived a Galactic birth rate of SNe Ia that is comparable to that inferred from observations. In the WD + MS channel obtained in Meng & Yang (2010b), the companion models are similar to those in Meng et al (2009). The masses stripped-off should then be similar to those found in Meng et al (2007), i.e., higher than 0.035 M .…”

Section: Introductionmentioning

confidence: 79%

The envelope mass of red giant donors in type Ia supernova progenitors

Meng¹,

Yang²

2010

A&A

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Context. The single degenerate model is the most widely accepted progenitor model of type Ia supernovae (SNe Ia), in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from a main sequence or a slightly evolved star (WD +MS) or from a red giant star (WD + RG), to increase its mass and explodes when approaching the Chandrasekhar mass. The explosion ejecta may impact the envelope of and strip off some hydrogen-rich material from the companion. The stripped-off hydrogen-rich material may manifest itself by means of a hydrogen line in the nebular spectra of SNe Ia. However, no hydrogen line is detected in the nebular spectra. Aims. We compute the remaining amounts of hydrogen in red giant donors to see whether the conflict between theory and observations can be overcome. Methods. By considering the mass-stripping effect from an optically thick wind and the effect of thermally unstable disk, we systematically carried out binary evolution calculation for WD + MS and WD + RG systems. Results. Here, we focus on the evolution of WD + RG systems. We found that some donor stars at the time of the supernova explosion contain little hydrogen-rich material on top of the helium core (as low as 0.017 M ), which is smaller than the upper limit to the amount derived from observations of material stripped-off by explosion ejecta. Thus, no hydrogen line is expected in the nebular spectra of these SN Ia. We also derive the distributions of the envelope mass and the core mass of the companions from WD + RG channel at the moment of a supernova explosion by adopting a binary population synthesis approach. We rarely find a RG companion with a very low-mass envelope. Furthermore, our models imply that the remnant of the WD + RG channel emerging after the supernova explosion is a single low-mass white dwarf (0.15−0.30 M ). Conclusions. The absence of a hydrogen line in nebular spectra of SNe Ia provides support to the proposal that the WD + RG system is the progenitor of SNe Ia.

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Section: Introductionmentioning

confidence: 79%

The envelope mass of red giant donors in type Ia supernova progenitors

Meng¹,

Yang²

2010

A&A

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“…The efficiency parameters η H and η He depend onṀ tr (Meng et al 2009). We refer to this wind as the Hachisu wind.…”

Section: Thermal Time-scale Mass Transfermentioning

confidence: 99%

“…2.6.3) and mass transfer might not be conservative during TTMT, we used the mass-transfer rate to distinguish between the CV phase and a phase of TTMT. We identify a binary as a system with TTMT if the primary is a WD, consisting of either helium (He), carbonoxygen (C/O), or oxygen-neon (O/Ne), the donor is a MS star and the mass-transfer rate is higher than the limit for stable hydrogen burning, as described in Meng et al (2009). Furthermore, the mass of the WD has to increase by at least 0.01 M during A143, page 2 of 14 the TTMT phase, otherwise we do not define the emerging CV as a post TTMT system.…”

Section: Mass Transfermentioning

confidence: 99%

White dwarf masses in cataclysmic variables

Wijnen

Zorotovic

Schreiber

2015

A&A

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Context. The white dwarf (WD) mass distribution of cataclysmic variables (CVs) has recently been found to dramatically disagree with the predictions of the standard CV formation model. The high mean WD mass among CVs is not imprinted in the currently observed sample of CV progenitors and cannot be attributed to selection effects. Two possibilities have been put forward to solve this issue: either the WD grows in mass during CV evolution, or in a significant fraction of cases, CV formation is preceded by a (short) phase of thermal time-scale mass transfer (TTMT) in which the WD gains a sufficient amount of mass. Aims. Here we investigate if and under which conditions a phase of TTMT before CV formation or mass growth in CVs can bring theoretical predictions and observations into agreement. Methods. We employed binary population synthesis models using the binary_c/nucsyn code to simulate the present intrinsic CV population. To that end we incorporated aspects specific to CV evolution such as an appropriate mass-radius relation of the donor star and a more detailed prescription for the critical mass ratio for dynamically unstable mass transfer. We have also implemented a previously suggested wind from the surface of the WD during TTMT and tested the idea of WD mass growth during the CV phase by arbitrarily changing the accretion efficiency. We compare the model predictions of the TTMT and the mass growth model with the characteristics of CVs derived from observed samples. Results. We find that mass growth of the WDs in CVs fails to reproduce the observed WD mass distribution. In the case of TTMT, we are able to produce a large number of massive WDs if we assume significant mass loss from the surface of the WD during the TTMT phase. However, the model still produces too many CVs with helium WDs. Moreover, the donor stars are evolved in many of these post-TTMT CVs, which contradicts the observations. Conclusions. We conclude that in our current framework of CV evolution neither TTMT nor WD mass growth can fully explain either the observed WD mass or the period distribution in CVs.

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“…However, for the low-metallicity cases, the WDs with a mass lower than 0.8 M may not contribute to SNe Ia (see Fig. 5 in Meng et al 2009). …”

Section: Resultsmentioning

confidence: 99%

“…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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A single-degenerate channel for the progenitors of Type Ia supernovae with different metallicities

Cited by 96 publications

References 123 publications

The envelope mass of red giant donors in type Ia supernova progenitors

The envelope mass of red giant donors in type Ia supernova progenitors

White dwarf masses in cataclysmic variables

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

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