Model-Synthesized Rate of Type Ia Supernovae and its Influence on the Chemical Enrichment of the ISM

Guo, Wen Bin; Zhang, Fenghui; Meng, Xiangcun; Li, Zhongmu; Han, Zhanwen

doi:10.1088/1009-9271/8/1/06

Cited by 3 publications

(5 citation statements)

References 33 publications

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“…However, the results above are opposite to the recent study of Guo et al (2008), where an analytic method was used (see also Hachisu et al 1999a,b; Nomoto et al 1999, 2003). Guo et al (2008) found that the peak of the birth rate for a low Z appears significantly earlier than that for a high Z . Also, they have not found the dependence of the peak value of birth rate on metallicity.…”

Section: The Results Of Binary Population Synthesiscontrasting

confidence: 76%

“…Thus, initial parameter spaces for SNe Ia are different in the two studies, i.e. a low metallicity leads to a higher maximum mass of the progenitors in Guo et al (2008). This tendency is the opposite of that in this paper.…”

Section: The Results Of Binary Population Synthesiscontrasting

confidence: 69%

“…For example, given Z = 0.02, the peak value from the analytic method is larger than that from detailed binary evolution calculations by a factor of 3, if a single starburst is assumed (Han & Podsiadlowski 2004). Note that our results are more physical than those obtained from the simple analytic method used by Hachisu et al (1999a,b), Nomoto et al (1999, 2003) and Guo et al (2008), as our results are based on detailed binary evolution calculations with the latest input physics.…”

Section: The Results Of Binary Population Synthesismentioning

confidence: 67%

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

Meng

Han

2009

Monthly Notices of the Royal Astronomical Society

133

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The single-degenerate channel for the progenitors of type Ia supernovae (SNe Ia) are currently accepted, in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from its companion, increases its mass to the Chandrasekhar mass limit, and then explodes as a SN Ia. Incorporating the prescription of Hachisu et al. (1999a) for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for all metallicities, we performed binary stellar evolution calculations for more than 25,000 close WD binaries with metallicities Z = 0.06, 0.05, 0.04, 0.03, 0.02, 0.01, 0.004, 0.001, 0.0003 and 0.0001. For our calculations, the companions are assumed to be unevolved or slightly evolved stars (WD + MS). As a result, the initial parameter spaces for SNe Ia at various Z are presented in orbital period-secondary mass (log P i , M i 2 ) planes. Our study shows that both the initial mass of the secondary and the initial orbital period increase with metallicity. Thus, the minimum mass of the CO WD for SNe Ia decreases with metallicity Z. The difference of the minimum mass may be as large as 0.24 M ⊙ for different Z.Adopting the results above, we studied the birth rate of SNe Ia for various Z via a binary population synthesis approach. If a single starburst is assumed, SNe Ia occur systemically earlier and the peak value of the birth rate is larger for a high Z. The Galactic birth rate from the WD + MS channel is lower than (but comparable to) that inferred from observations. Our study indicates that supernovae like SN2002ic would not occur in extremely low-metallicity environments, if the delayed dynamicalinstability model in Han & Podsiadlowski (2006) is appropriate.

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Section: The Results Of Binary Population Synthesiscontrasting

confidence: 76%

Section: The Results Of Binary Population Synthesiscontrasting

confidence: 69%

Section: The Results Of Binary Population Synthesismentioning

confidence: 67%

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

Meng

Han

2009

Monthly Notices of the Royal Astronomical Society

133

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“…The first reason lies in the chemical evolution of galaxies, because they synthesize additional heavy elements, which are distributed among the pre-explosion stars. Type Ia's provide more than half of the iron-peak elements and some intermediate mass (carbon-sulfur) material (Guo et al 2008;Matteucci 2010;Jiménez et al 2015;Simionescu et al 2015). The core collapse events generate everything from helium to iron, and also elements beyond iron from slow neutron capture in the parent stars and probably from rapid neutron capture in the event itself.…”

Section: Supernovaementioning

confidence: 99%

Rubin Observatory LSST Transients and Variable Stars Roadmap

Hambleton,

Bianco,

Street

et al. 2023

PASP

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The Vera C. Rubin Legacy Survey of Space and Time (LSST) holds the potential to revolutionize time domain astrophysics, reaching completely unexplored areas of the Universe and mapping variability time scales from minutes to a decade. To prepare to maximize the potential of the Rubin LSST data for the exploration of the transient and variable Universe, one of the four pillars of Rubin LSST science, the Transient and Variable Stars Science Collaboration, one of the eight Rubin LSST Science Collaborations, has identified research areas of interest and requirements, and paths to enable them. While our roadmap is ever-evolving, this document represents a snapshot of our plans and preparatory work in the final years and months leading up to the survey’s first light.

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“…A series of works searching for variables in clusters has been performed up to now (Lü et al 2006(Lü et al , 2007Xin et al 2002;Zhang et al 2003, 2005Li et al 2004Li et al 2004bLi et al 2004a). Moreover, binaries (a white dwarf + an MS or red giant) are believed to be possible progenitors of type Ia supernovae (Meng et al 2006(Meng et al , 2009Wang et al 2008Wang et al , 2010Wang & Han 2010a,b;Guo et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Modeling blue stragglers in young clusters

Lu¹,

Deng²,

Zhang³

2011

Res. Astron. Astrophys.

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In this paper, a grid of the binary evolution models are calculated for the study of blue straggler (BS) population in intermediate age ) star clusters. The BS formation via mass transfer and merging is studied systematically using our models. Both Case A and B close binary evolutionary tracks are calculated in a large range of parameters.The results show that BSs formed via Case B are generally bluer and even more luminous than those produced by Case A. Furthermore, the larger range in orbital separations of Case B models provide a probability of producing more BSs than Case A. Based on the grid of models, several Monte-Carlo simulations of BS populations in the clusters in the age range are carried out. The results show that BSs formed via different channels populate different areas in color magnitude diagram(CMD). The locations of BSs in CMD for a number of clusters are compared to our simulations as well. In order to investigate the influence of mass transfer efficiency in the models and simulations, a set of models are also calculated by implementing a constant mass transfer efficiency, β=0.5 during Roche lobe overflow (Case A binary evolution excluded). The result shows BSs can be formed via mass transfer at any given age in both cases. However, the distributions of the BS populations on CMD are different.

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Model-Synthesized Rate of Type Ia Supernovae and its Influence on the Chemical Enrichment of the ISM

Cited by 3 publications

References 33 publications

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

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

Rubin Observatory LSST Transients and Variable Stars Roadmap

Modeling blue stragglers in young clusters

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