Volume 515, June 2010
|Number of page(s)||6|
|Section||Stellar structure and evolution|
|Published online||11 June 2010|
The helium star donor channel for the progenitors of type Ia supernovae with different metallicities
National Astronomical Observatories/Yunnan Observatory,
the Chinese Academy of Sciences, Kunming 650011, PR China e-mail: [wangbo;zhanwenhan]@ynao.ac.cn
2 Key Laboratory for the Structure and Evolution of Celestial Objects, the Chinese Academy of Sciences, Kunming 650011, PR China
3 Graduate University of the Chinese Academy of Sciences, Beijing 100049, PR China
Accepted: 18 March 2010
Context. The nature of type Ia supernovae (SNe Ia) is still unclear. Metallicities may have an important effect on their properties.
Aims. In this paper, we study the He star donor channel towards SNe Ia comprehensively and systematically at various metallicities.
Methods. Employing Eggleton's stellar evolution code with the optically thick wind assumption, we calculated about 10 000 WD + He star systems and obtained SN Ia production regions of the He star donor channel with metallicities Z = 0.03, 0.02, 0.004 and 0.0001. According to a detailed binary population synthesis approach, we also obtained SN Ia birthrates at various metallicities.
Results. Our study shows that both the initial mass of the He donor star and the initial orbital period for SNe Ia increase with metallicity, while the minimum initial mass of the carbon–oxygen white dwarfs producing SNe Ia decreases with metallicity. For a constant star-formation galaxy, SN Ia birthrates increase with metallicity. If a single starburst is assumed, SNe Ia occur systemically earlier and the peak value of the birthrate is larger for a high Z, and the He star donor channel with different metallicities can produce the young SNe Ia with delay times ~45–220 Myr.
Key words: binaries: close / supernovae: general / white dwarfs / stars: evolution
© ESO, 2010
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