Radial-Velocity Variability of G-Type Giants: First Three Years of the Okayama Planet Search Program
Radial-Velocity Variability of G-Type Giants: First Three Years of the Okayama Planet Search Program
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DOI：
10.1093/pasj/57.1.97
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发表时间：
2005-02
影响因子：
2.3
通讯作者：
B. Sato;E. Kambe;Y. Takeda;H. Izumiura;S. Masuda;H. Ando
中科院分区：
文献类型：
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作者：
B. Sato;E. Kambe;Y. Takeda;H. Izumiura;S. Masuda;H. Ando
我们根据冈山行星搜索计划前 3 年观测到的 57 颗恒星的精确多普勒测量结果，报告了 G 型巨星的径向速度变化。该计划旨在寻找处于晚期G巨星演化阶段的中等质量恒星周围的行星。我们发现大多数 B −V 1.0 的目标通常显示 σ ∼ 20ms−1。总共，在 4 颗恒星（HD 41597、HD 134190、HD 161178 和 HD 176598）中发现约 60% 的目标在径向速度上稳定在 σ 30ms−1 的水平。对于大多数没有表现出任何显着周期性的恒星，我们可以排除 K > 50ms−1 或 m2 sin i > 1.8MJ(a/AU)(M*/M )1/2 的伴星，轨道半径 a 1–2AU。
We report on the radial-velocity variability of G-type giants based on the results of precise Doppler measurements of 57 stars that were observed for the first 3 years of the Okayama Planet Search Program. This program aims to search for planets around intermediate-mass stars in their evolved stages as late-G giants. We found that most of the targets with B −V 1.0 typically show σ ∼ 20ms−1. In total, about 60% of the targets are stable in radial velocity to a level of σ 30ms−1 are found in 4 stars (HD 41597, HD 134190, HD 161178, and HD 176598). For most of the stars without showing any significant periodicity, we can exclude companions with K > 50ms−1, or m2 sin i > 1.8MJ(a/AU)(M∗/M )1/2 for orbital radii a 1–2AU.