权益分类	功能权益	普通用户	{{item.name}}会员
{{category.name}}	{{benefitItem.name}}

Quantitative Spectroscopic Analyses of Chemically Peculiar Stars in the UV and Near-IR Regions

紫外和近红外区域化学特殊恒星的定量光谱分析

基本信息

批准号：
61540184
负责人：
SADAKANE Kouzou
金额：
$ 0.96万
依托单位：
Osaka Kyoiku University
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (C)
财政年份：
1986
资助国家：
日本
起止时间：
1986 至 1988
项目状态：
已结题

项目摘要

(1) High resolution ultraviolet spsectroscopic data of early type stars including CP stars are analyzed quantitatively. They were obtained with the IUE and Copernicus satellites. Resonance lines of Ga II and Ga III in B-type CP stars were analyzed and anomalous abundances of Ga were found not only in Hg-Mn stars but also in magnetic (Si type) stars (M. Takada-Hidai, K. Sadakane, and J. Jugaku, 1986, Ap. J., 304, 425). The resonance line of Zn II at 2062 A in Hg-Mn stars was analyzed using the spectrum synthsis method. A remarkable variation in the abundance of Zn was found among Hg-Mn stars (K. Sadakane, J. Jugaku, and M. Takada-Hidai, 1988, Ap. J., 325, 776). The resonance line of Hg II at 1942 A in Sirius and Vega was analyzed and Hg in Vega was found to be under-abundant with respect to the solar system abundance (K. Sadakane, J. Jugaku, and M. Takada-Hidai, 1988, P. A. S. P., 100, 811).(2) High S/N ratio spectra of 12 A-type stars in the 8700 A region were obtained using a CCD detector at the Okayama Astrophysical Observatory. Absorption lines of N I and S I were analyzed for their abundances in these 12 stars using model atmospheres. Abundances of both N and S are found to be normal in most stars while they both are underabundat in the two CP stars (73 DMa and UMa). Details will be published shortly (K. Sadakane and M.Okyudo, 1989, submitted to P. A. S. Japan).

(1)对包括CP星在内的早型星的高分辨紫外光谱数据进行了定量分析。它们是由IUE和哥白尼卫星获得的。分析了B型CP星中Ga Ⅱ和Ga Ⅲ的共振线，发现Ga不仅在Hg-Mn星中，而且在磁性（Si型）星中也存在异常丰度。Takada-Hidai，K. Sadakane，and J. Jugaku，1986，Ap. J.，304、425）。用光谱分析方法对Hg-Mn星中Zn Ⅱ的2062 A共振线进行了分析。在Hg-Mn星中，Zn的丰度存在着显著的差异（K. Sadakane，J. Jugaku，and M. Takada-Hidai，1988，Ap. J.，325，776）。分析了天狼星和织女星中1942 A时Hg II的共振线，发现织女星中Hg的丰度相对于太阳系的丰度（K. Sadakane，J. Jugaku，and M. Takada-Hidai，1988，P. A. S. P.，100，811）。(2)利用冈山天体物理观测站的CCD探测器获得了8700 A区12颗A型星的高信噪比光谱。利用模型大气分析了这12颗恒星的NI和SI吸收线丰度。在大多数恒星中N和S的丰度都是正常的，而在两颗CP星（73 DMa和UMa）中N和S的丰度都是偏低的。详情将于稍后公布（K。Sadakane和M.Okyudo，1989年，提交给P.A. S.日本）。