Oscillations in G-Type Giants

被引:8
作者
Ando, Hiroyasu [1 ,2 ,3 ]
Tsuboi, Yusuke [3 ]
Kambe, Eiji [4 ]
Sato, Bun'ei [5 ]
机构
[1] Natl Inst Nat Sci, Natl Astron Observ Japan, Tokyo 1818588, Japan
[2] Grad Univ Adv Studies, Dept Astron, Kanagawa 2400193, Japan
[3] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan
[4] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama, Japan
[5] Tokyo Inst Technol, Meguro Ku, Tokyo 1528550, Japan
基金
日本学术振兴会;
关键词
stars: G-type giants: asteroseismdogy; stars: oscillations; stars: variables; techniquies: radial velocities; SOLAR-LIKE OSCILLATIONS; RED GIANTS; STELLAR PARAMETERS; ANGULAR DIAMETERS; MODE LIFETIME; STARS; ASTEROSEISMOLOGY; ABUNDANCES; LUMINOSITY; COMPANION;
D O I
10.1093/pasj/62.4.1117
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Precise radial-velocity measurements of 4 G-type giants, 11 Corn, zeta Hya, epsilon Tau, and eta Her, were carried out. Short-term variations with amplitudes of 1-7 ms(-1) and periods of 3-10 hr were detected. A period analysis shows that the individual power distribution has a Gaussian shape, and that their peak frequencies (nu(max)) are in a good agreement with a prediction by the scaling law. With using a pre-whitening procedure, significant frequency peaks of more than 3 sigma were extracted for these giants. From these peaks, we determined the large frequency separation by constructing the highest peak distribution of the collapsed power spectrum, which is also in good agreement with what the scaling law for the large separation predicts. Echelle diagrams of the oscillation frequency were created based on the extracted large separations, which is very useful to clarify the properties of the oscillation modes. In these echelle diagrams, odd-even mode sequences are clearly seen. Therefore, it is certain that in these G-type giants, non-radial modes are detected in addition to the radial mode. As a consequence, these properties of oscillation modes are shown to follow what Dziembowski et al. (2001, MNRAS, 328, 601) and Dupret et al. (2009, A&A, 506, 57) theoretically predicted. The damping times for these giants were estimated with the same method as that developed by Stello et al. (2004, Sol. Phys., 220, 207). The relation of the Q-value (ratio of damping time to period) to the period was discussed by adding data of other stars, ranging from dwarfs to giants.
引用
收藏
页码:1117 / 1126
页数:10
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