Initial-final mass relationship for stars of different metallicities

Meng, Xingmin; Chen, X.; Han, Zhanwen

doi:10.1051/0004-6361:20078841

Cited by 101 publications

(132 citation statements)

References 98 publications

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“…Too long to compare with our simulation (see Fig. 1), the orbital period leads to a lower envelope binding energy than produced by the model developed in this paper since the binding energy of the envelope is determined mainly by the radius of the RG star (Meng et al 2008). The envelope of the RG model used by Marietta et al (2000) is then more likely to be stripped off and the amount of material stripped-off by the RG companion in Marietta et al (2000) might be overestimated.…”

Section: Interaction Between Supernova Ejectamentioning

confidence: 88%

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: Interaction Between Supernova Ejectamentioning

confidence: 88%

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

Meng¹,

Yang²

2010

A&A

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“…Therefore, the amount of work necessary to eject completely the stellar envelopes of massive AGB stars is much higher and, even though our panels showing the binding energy profiles seem to point to the disruption of the star, we cannot discard an eventual fallback of the envelopes. We have calculated the envelope binding energy for the last computed models as Meng et al (2008), and obtained a result of −3 × 10 45 erg. This value is negative and, therefore technically the envelope still remains bound.…”

Section: What Will Happen To the Star?mentioning

confidence: 99%

The end of super AGB and massive AGB stars

Lau

Gil‐Pons

Doherty

et al. 2012

A&A

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Context. The literature is rich in analysis and results related to thermally pulsing-asymptotic giant branch (TP-AGB) stars, but the problem of the instabilities that arise and cause the divergence of models during the late stages of their evolution is rarely addressed. Aims. We investigate the physical conditions, causes and consequences of the interruption in the calculations of massive AGB stars in the late thermally-pulsing AGB phase. Methods. We have thoroughly analysed the physical structure of a solar metallicity 8.5 M star and described the physical conditions at the base of the convective envelope (BCE) just prior to divergence. Results. We find that the local opacity maximum caused by M-shell electrons of Fe-group elements lead to the accumulation of an energy excess, to the departure of thermal equilibrium conditions at the base of the convective envelope and, eventually, to the divergence of the computed models. For the 8.5 M case we present in this work the divergence occurs when the envelope mass is about 2 M . The remaining envelope masses range between somewhat less than 1 and more than 2 M for stars with initial masses between 7 and 10 M and, therefore, our results are relevant for the evolution and yields of super-AGB stars. If the envelope is ejected as a consequence of the instability we are considering, the occurrence of electron-capture supernovae would be avoided at solar metallicity.

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“…When a star evolves to the stage, its envelope may be lost if the binding energy (BE) of the envelope transforms from a negative phase to a positive one (Paczyński & Ziólkowski 1968; see also Fig. 2 in Meng et al 2008). We calculated the BE of the envelope to be…”

Section: Methodsmentioning

confidence: 99%

“…Here, we assume that a star will lose its envelope when the BE of the star's envelope increases to the point of ΔW = 0 and the core mass at the point is the final WD mass. The method here is robust and its virtue is significant because we need not consider the specific mechanism of mass loss since the mass loss rate is very uncertainty (see Meng et al 2008, in details about this method). We assume that after envelope ejection the remnant is a CO WD if carbon and oxygen have not been ignited at the moment of envelope ejection.…”

Section: Methodsmentioning

confidence: 99%

“…This treatment of the thermal pulses may miss some information about the structural change of the envelope due to the thermal pulse. However, these treatment will not affect our final results because the situation of ΔW = 0 is fulfilled before the onset of thermal pulse and after the point a simple assumption of C/O = 1 is adopted (see also in Meng et al 2008).…”

Section: Methodsmentioning

confidence: 99%

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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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Initial-final mass relationship for stars of different metallicities

Cited by 101 publications

References 98 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

The end of super AGB and massive AGB stars

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

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