Type Ia Supernovae: Progenitors and Diversities

Nomoto, K.; Uenishi, Tatsuhiro; Kobayashi, Chiaki; Umeda, Hideyuki; Ohkubo, Takuya; Hachisu, Izumi; Kato, Mariko

doi:10.1007/10828549_16

Cited by 68 publications

(58 citation statements)

References 42 publications

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“…In this model, a CO WD increases its mass by accreting hydrogen-or helium-rich matter from its companion, and explodes when its mass approaches the Chandrasekhar mass limit. The companion may be a main-sequence star (WD+MS) or a red-giant star (WD+RG) (Yungelson et al 1995;Li et al 1997;Hachisu et al 1999a,b;Nomoto et al 1999Nomoto et al , 2003Langer et al 2000;Han & Podsiadlowski 2004;Chen & Li 2007Han 2008;Meng et al 2009;Meng & Yang 2010a;Lü 2009;Wang et al 2009bWang et al , 2009cWang et al , 2010. The SD model has also been verified by many observations (see Meng & Yang 2010b).…”

Section: Introductionmentioning

confidence: 80%

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: 80%

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

Meng¹,

Yang²

2010

A&A

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“…A different ejection channel is provided by the SN Ia that are believed to arise from thermonuclear explosions of white dwarfs (WD hereafter) in binary stellar systems as a consequence of the matter accretion from the companion (e.g., Nomoto et al 2000). However, there are still a number of uncertainties about the nature of both the WD and the companion and about the mass reached at the onset of the explosion (e.g., Matteucci and Recchi 2001;Yungelson and Livio 2000).…”

Section: What Is a Model Of Chemical Evolution?mentioning

confidence: 99%

“…Following Greggio and Renzini (1983), we assume here that SN Ia arise from stars belonging to binary systems, having mass in the range 0.8-8 M . Accordingly, in the single-degenerate WD scenario (Nomoto et al 2000), the rate of explosions of SN Ia can be written as…”

Section: Type Ia Supernovaementioning

confidence: 99%

The Chemical Enrichment of the ICM from Hydrodynamical Simulations

et al. 2008

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The study of the metal enrichment of the intra-cluster and inter-galactic media (ICM and IGM) represents a direct means to reconstruct the past history of star formation, the role of feedback processes and the gas-dynamical processes which determine the evolution of the cosmic baryons. In this paper we review the approaches that have been followed so far to model the enrichment of the ICM in a cosmological context. While our presentation will be focused on the role played by hydrodynamical simulations, we will also discuss other approaches based on semi-analytical models of galaxy formation, also critically discussing pros and cons of the different methods. We will first review the concept of the model of chemical evolution to be implemented in any chemo-dynamical description. We will emphasise how the predictions of this model critically depend on the choice of the stellar initial mass function, on the stellar life-times and on the stellar yields. We will then overview the comparisons presented so far between X-ray observations of the ICM enrichment and model predictions. We will show how the most recent chemo-dynamical models are able to capture the basic features of the observed metal content of the ICM and its evolution. We will conclude by highlighting the open questions in this study and the direction of improvements for cosmological chemo-dynamical models of the next generation.

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“…However, the metallicity dose not seem to have the ability to interpret the whole scatter in the maximum luminosity of SNe Ia (Timmes et al 2003;Gallagher et al 2008;Howell et al 2009b). Nomoto et al (1999Nomoto et al ( , 2003 suggested that the average 1 ratio of carbon to oxygen (C/O) of a white dwarf at the moment of explosion is the dominant parameter of the Phillips relation (see also Umeda et al 1999b). The higher the C/O, the larger the amount of nickel-56, and then the higher the maximum luminosity of SNe Ia.…”

Section: Introductionmentioning

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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Type Ia Supernovae: Progenitors and Diversities

Cited by 68 publications

References 42 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 Chemical Enrichment of the ICM from Hydrodynamical Simulations

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

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