Initial-final mass relationship for stars of different metallicities

	Initial-final mass relationship for stars of different metallicities
	Meng XC(孟祥存)1,2 ; Chen XF(陈雪飞)1 ; Han ZW(韩占文)1
刊名	ASTRONOMY & ASTROPHYSICS
	2008-08
卷号	487 期号:2 页码:625-635
关键词	stars : white dwarfs stars : supernovae : general
ISSN号	0004-6361
通讯作者	Meng, X (reprint author), Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China.
产权排序	第一完成单位
英文摘要	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.
学科主题	Astronomy & Astrophysics
WOS标题词	Science & Technology ; Physical Sciences
类目[WOS]	Astronomy & Astrophysics
研究领域[WOS]	Astronomy & Astrophysics
关键词[WOS]	ASYMPTOTIC GIANT BRANCH ; OPEN CLUSTER NGC-6791 ; DWARF COOLING SEQUENCES ; VERY-LOW-MASS ; WHITE-DWARF ; IA SUPERNOVAE ; STELLAR EVOLUTION ; SOLAR NEIGHBORHOOD ; LUMINOSITY FUNCTIONS ; GLOBULAR-CLUSTERS
收录类别	SCI ; EI
原文出处	http://www.aanda.org/articles/aa/abs/2008/32/aa8841-07/aa8841-07.html
语种	英语
WOS记录号	WOS:000258327900033
内容类型	期刊论文
源URL	[http://ir.ynao.ac.cn/handle/114a53/4449]
专题	云南天文台_大样本恒星演化研究组
作者单位	1.National Astronomical Observatories/Yunnan Observatory, the Chinese Academy of Sciences, Kunming, 650011, PR China 2.Graduate School of the Chinese Academy of Sciences, PR China
推荐引用方式 GB/T 7714	Meng XC,Chen XF,Han ZW. Initial-final mass relationship for stars of different metallicities[J]. ASTRONOMY & ASTROPHYSICS,2008,487(2):625-635.
APA	Meng XC,Chen XF,&Han ZW.(2008).Initial-final mass relationship for stars of different metallicities.ASTRONOMY & ASTROPHYSICS,487(2),625-635.
MLA	Meng XC,et al."Initial-final mass relationship for stars of different metallicities".ASTRONOMY & ASTROPHYSICS 487.2(2008):625-635.