Studies on properties of planet-host stars and on formation conditions of planets based on analyses of chemical compositions.

基于化学成分分析研究行星宿主恒星的性质和行星的形成条件。

• 批准号: 22540255
• 负责人: HIDAI Masahide
• 金额: $ 1.83万
• 依托单位: Tokai University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2010
• 资助国家: 日本
• 起止时间: 2010 至 2012
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-22540255/
• 关键词: 光学赤外線天文学; 惑星形成; 元素組成; 金属度; 惑星探査; 分光観測; 巨星; 矮星; 化学組成; 恒星分光学; G型巨星; 系外惑星; 金属欠乏星; 褐色矮星; M型矮星

Abundance analyses of 13 elements (C to Zn) were carried out for 73 planet-host starsand 18 comparison stars. Comparison of [Fe/H] with a total metallicity [M/H] which includes abundances of Fe and 13 elements yielded the result that [M/H] corresponds to about 0.75 of [Fe/H] value, and suggested that [M/H] should be used as a metallicity concerning a condition for planet formation in the metal-deficient region. One hot Jupiter was detected around one intermediate-mass giant by planet survey, and its mass was turned out to be a new lower limit of planets being formed around intermediate-mass stars. It is found that about 10 stars of the giant sample may have planet around them, and that Fe abundances distribute around the solar value, which is different from dwarfs case. As for the related studies, behaviors of sulfur and silicon of alpha elements and existence of chromosphere were investigated in the sample of metal-poor dwarfs and giants. Sulfur shows a flat trend with +0.4 dex against [Fe/H] in a lower metallicity region. Silicon shows a behavior similar to sulfur, but it is confirmed that NLTE analyses are necessary for abundance analyses based on near infrared absorption lines. As for chromosphere, it is confirmed observationally that chromosphere exists in dwarfs and giants commonly independent of metallicity.

对73个行星宿主星和18个比较星进行了13个元素（C至Zn）的丰度分析。 [Fe/H]与总金属性[M/H]的比较，其中包括Fe的丰度和13个元素，结果[M/H]对应于[Fe/H]值的约0.75，并建议将[M/H]用作金属缺陷区域中Planet形成的金属条件。通过行星调查发现了一个热木星在一个中间质量巨人周围发现，事实证明它的质量是中间质量恒星周围形成的新的下限。发现大约有10颗巨大样本的恒星可能周围有行星，而Fe丰度则分布在太阳值周围，这与矮人的情况不同。至于相关研究，在金属贫困矮人和巨人的样本中研究了α元素硫和硅的行为。硫显示在较低的金属区域中对[Fe/H]的+0.4 DEX的平坦趋势。硅显示了类似于硫的行为，但可以证实，基于近红外吸收系的丰度分析是必需的。至于染色体，从矮人和巨人中存在染色体，通常与金属性无关。

项目成果

Behavior of [S/Fe] in Very Meta-Poor Stars from the SI 1.046 μm Lines Revisited

重新审视 SI 1.046 μm 谱线中非常贫乏恒星中的 [S/Fe] 行为

• 发表时间: 2012
• 期刊: Pub. Astron.Soc.Japan
• 作者: Takeda;Y. & Takada-Hidai;M.
• 通讯作者: M.

IRDチームすばるIRDによるサイエンス:M型矮星の観測

IRD 团队 Subaru IRD 的科学：M 型矮星的观测

• 发表时间: 2011
• 作者: 青木和光;西山正吾;森野潤一;大宮正士;比田井昌英;末永拓也
• 通讯作者: 末永拓也

SILICON ABUNDANCES IN NEARBY STARS FROM THE Si i INFRARED LINES

• DOI: 10.1088/0004-637x/755/1/36
• 发表时间: 2012-07
• 期刊: The Astrophysical Journal
• 作者: Jian-rong Shi;M. Takada-Hidai;Y. Takeda;K. Tan;Shaoming Hu;Gang Zhao;Chen Cao

G型巨星における惑星系の日韓共同探査.VII

日韩联合探索G型巨星行星系统七

• 发表时间: 2011
• 作者: 大 宮 正 士 ;....比田井昌英;他
• 通讯作者: 他

中性硫黄の近赤外3重線に基づく金属欠乏星の硫黄組成の振る舞い

基于中性硫近红外三重态的缺金属恒星中硫成分的行为

• 发表时间: 2011
• 作者: 比田井昌英;竹田洋一
• 通讯作者: 竹田洋一