A Jupiter-mass planet around the K0 giant HD 208897

被引：7

作者：

Yilmaz, M. ^{[1
]}

Sato, B. ^{[2
]}

Bikmaev, I. ^{[3
,6
]}

Selam, S. O. ^{[1
]}

Izumiura, H. ^{[4
]}

Keskin, V. ^{[5
]}

Kambe, E. ^{[4
]}

Melnikov, S. S. ^{[3
,6
]}

Galeev, A. ^{[3
,6
]}

Ozavci, I. ^{[1
]}

Irtuganov, E. N. ^{[3
,6
]}

Zhuchkov, R. Ya. ^{[3
,6
,7
]}

机构：

[1] Ankara Univ, Dept Astron & Space Sci, TR-06100 Ankara, Turkey

[2] Tokyo Inst Technol, Meguro Ku, Tokyo 1528550, Japan

[3] Kazan Fed Univ, Dept Astron & Satellite Geodesy, Kazan 420008, Russia

[4] Okayama Astrophys Observ, Honjo 3037-5, Asakuchi, Okayama 7190232, Japan

[5] Ege Univ, Dept Astron & Space Sci, TR-35100 Izmir, Turkey

[6] Acad Sci Tatarstan, Bauman Str 20, Kazan 420111, Russia

[7] Russian Acad Sci, Main Pulkovo Astron Observ, St Petersburg 196140, Russia

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 608卷

关键词：

stars: individual: HD 208897; planetary systems; stars: fundamental parameter; techniques: radial velocities; STARS; COMPANIONS; EVOLUTION; DISTRIBUTIONS; METALLICITY; ABUNDANCES;

D O I：

10.1051/0004-6361/201731184

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

For over 10 years, we have carried out a precise radial velocity (RV) survey to find substellar companions around evolved G, K-type stars to extend our knowledge of planet formation and evolution. We performed high precision RV measurements for the giant star HD 208897 using an iodine (l(2)) absorption cell. The measurements were made at TUBlTAK National Observatory (TUG; RTT150) and Okayama Astrophysical Observatory (OAO). For the origin of the periodic variation seen in the RV data of the star, we adopted a Keplerian motion caused by an unseen companion. We found that the star hosts a planet with a minimum mass of m(2) sin i = 1.40 M-J, which is relatively low compared to those of known planets orbiting evolved intermediate-mass stars. The planet is in a nearly circular orbit with a period of P = 353 days at about 1 AU distance from the host star. The star is metal rich and located at the early phase of ascent along the red giant branch. The photometric observations of the star at Ankara University Kreiken Observatory (AUKR) and the HlPPARCOS photometry show no sign of variation with periods associated with the RV variation. Neither bisector velocity analysis nor analysis of the Ca II and H alpha lines shows any correlation with the RV measurements.

引用

页数：8

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