Initial-final mass relationship for stars of different metallicities
Initial-final mass relationship for stars of different metallicities
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不同金属丰度恒星的初始-最终质量关系
DOI：
10.1051/0004-6361:20078841
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发表时间：
2007-10
影响因子：
6.5
通讯作者：
陈雪飞
中科院分区：
文献类型：
--
作者：
韩占文;孟祥存;陈雪飞
上下文。恒星的初始-最终质量关系（IFMR）在许多天体物理研究领域都很重要，例如星系的演化、Ia型超新星（SNe Ia）的性质和星系中暗物质的组成。目标。本文的目的是得到IFMR对金属丰度的依赖关系。方法。假设渐近巨支（AGB）或第一巨支（FGB）恒星的包络层在包络层结合能等于零（W = 0）时失去，取AGB恒星或FGB恒星在该点（W = 0）处的核心质量作为最终质量。利用这一假设，我们计算了不同金属丰度恒星的ifmr。结果。我们发现IFMR强烈依赖于金属丰度，即Z = 0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02, 0.03, 0.04, 0.05, 0.06, 0.08和0.1。从Z = 0.04开始，具有给定初始质量的恒星的最终质量随着金属丰度的增加或减少而增加。由于金属丰度导致的最终质量差异可达0.4 M（圆点）。ngc2099 （M37）的初始-最终质量关系的线性拟合显示了金属丰度对IFMR的影响。这里得到的Z = 0.02恒星的IFMR与银河系中观测推断的结果吻合得很好。对于Z >= 0.02，氦WDs来自M(i) <= 1.0 M（圆点）的恒星，这一结果得到了NGC 6791中大量低质量WDs的发现的支持，NGC 6791是一个富含金属的古老疏散星团。利用这里得到的Z = 0.02恒星的IFMR，我们重现了Sloan DR4中除了一些超大质量白矮星外的DA WDs的质量分布。结论。wds的平均质量随有效温度的增加而减小的趋势可能源于恒星初始金属丰度的增加。我们简要地讨论了IFMR对Ia超新星的潜在影响，同时预测富含金属的低质量恒星可能成为低质量白矮星。
Context. The initial-final mass relationship (IFMR) for stars is important in many astrophysical fields of study, such as the evolution of galaxies, the properties of type Ia supernovae (SNe Ia) and the components of dark matter in the Galaxy. Aims. The purpose of this paper is to obtain the dependence of the IFMR on metallicity. Methods. We assume that the envelope of an asymptotic giant branch (AGB) or a first giant branch (FGB) star is lost when the binding energy of the envelope is equal to zero (Delta W = 0) and the core mass of the AGB star or the FGB star at the point (Delta W = 0) is taken as the final mass. Using this assumption, we calculate the IFMRs for stars of different metallicities. Results. We find that the IFMR depends strongly on the metallicity, i.e. Z = 0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02, 0.03, 0.04, 0.05, 0.06, 0.08 and 0.1. From Z = 0.04, the final mass of the stars with a given initial mass increases with increasing or decreasing metallicity. The difference in the final mass due to the metallicity may be up to 0.4 M(circle dot). A linear fit of the initial-final mass relationship in NGC 2099 (M37) shows the effect of metallicity on the IFMR. The IFMR for stars of Z = 0.02 obtained here matches well with those inferred observationally in the Galaxy. For Z >= 0.02, helium WDs are obtained from the stars of M(i) <= 1.0 M(circle dot) and this result is supported by the discovery of numerous low-mass WDs in NGC 6791, which is a metal-rich old open cluster. Using the IFMR for stars of Z = 0.02 obtained here, we have reproduced the mass distribution of DA WDs in Sloan DR4 except for some ultra-massive white dwarfs. Conclusions. The trend that the mean mass ofWDs decreases with effective temperature may originate from the increase of the initial metallicities of stars. We briefly discuss the potential effects of the IFMR on SNe Ia and at the same time, predict that metal-rich low-mass stars may become under-massive white dwarfs.
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DOI：
10.1086/116601
发表时间：
1993-06
期刊：
The Astronomical Journal
影响因子：
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通讯作者：
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影响因子：
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作者：
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DOI：
10.1046/j.1365-8711.2002.05038.x
发表时间：
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影响因子：
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