Chemical abundances of 22 extrasolar planet host stars

	Chemical abundances of 22 extrasolar planet host stars
	Huang, C.; Zhao, G.; Zhang, H. W.; Chen, Y. Q.
刊名	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
	2005-10-11
卷号	363 期号:1 页码:71-78
关键词	star : abundances star : late-type planetary systems
英文摘要	We present observations of 22 extrasolar planet host stars and derive their stellar parameters. With the high signal-to-noise ratio spectra, we acquire accurate metallicities and the differential abundances for 15 other elements and we discuss the relation between the abundance ratio and the metallicity. These sample stars are metal-rich relative to the Sun, covering the range from -0.04 to 0.54 dex with the average [Fe/H] value of 0.15 +/- 0.12 dex, except for HD 37124, which has [Fe/H] = -0.45. The stars with planets show a slight overabundance pattern for [C/Fe] and [Mg/Fe], but [Na/Fe], [Al/Fe], [Si/Fe], [Ti/Fe], [Cr/Fe], [Sc/Fe], [V/Fe], [Ni/Fe] and [Ba/Fe] are approximately solar in the sample stars. These stars also show slight underabundances for [O/Fe], [Ca/Fe] and [Mn/Fe]. The sulphur displays enhanced values, ranging from -0.10 to 0.40 through the sample stars. These results are used to investigate the connection between giant planets and high metallicity and to probe the influence of the process on the other elements.
收录类别	SCI
语种	英语
WOS记录号	WOS:000232168100007
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/7020]
专题	国家天文台_光学天文研究部
作者单位	1.Peking Univ, Dept Astron, Beijing 100871, Peoples R China 2.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
推荐引用方式 GB/T 7714	Huang, C.,Zhao, G.,Zhang, H. W.,et al. Chemical abundances of 22 extrasolar planet host stars[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2005,363(1):71-78.
APA	Huang, C.,Zhao, G.,Zhang, H. W.,&Chen, Y. Q..(2005).Chemical abundances of 22 extrasolar planet host stars.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,363(1),71-78.
MLA	Huang, C.,et al."Chemical abundances of 22 extrasolar planet host stars".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 363.1(2005):71-78.