Detection of a planetary companion around the giant star γ1 Leonis

By I. Han, Byeong-Cheol Lee, Kang-Min Kim, D. Mkrtichian, A. Hatzes, G. Valyavin. 2009

224 citations recorded by the source corpus.

Aims. Our primary goal is to search for planets around intermediate mass stars. We are also interested in studying the nature of radial velocity (RV) variations of K giant stars. Methods. We selected about 55 early K giant (K0-K4) stars brighter than fifth magnitude that were observed using BOES, a high resolution spectrograph attached to the 1.8 m telescope at BOAO (Bohyunsan Optical Astronomy Observatory). BOES is equipped with I 2 absorption cell for high precision RV measurements. Results. We detected a periodic radial velocity variations in the K0 III star γ 1 Leonis with a period of P = 429 days. An orbital fit of the observed RVs yields a period of P = 429 days, a semi-amplitude of K = 208 m s -1 , and an eccentricity of e = 0.14. To investigate the nature of the RV variations, we analyzed the photometric, Ca II λ 8662 equivalent width, and line-bisector variations ofy' Leonis . We conclude that the detected RV variations can be best explained by a planetary companion with an estimated mass of m sin i = 8.78 M Jupiter and a semi-major axis of α = 1.19 AU, assuming a stellar mass of 1.23 M ⊙ .

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/e7fafca608ad16f93215772c28d23913f6467213

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In Astronomy and Astrophysics

1. C. Mordasini
2. Th. Henning
3. Y. Alibert
4. H. Klahr
5. W. Benz
6. Sheng Jin
7. Anders Johansen
8. A. Morbidelli

In Instrumentation

1. C. Mordasini
2. Th. Henning
3. Y. Alibert
4. W. Benz
5. H. Klahr
6. Sheng Jin
7. R. van Boekel

In Statistical and Nonlinear Physics

1. C. Mordasini
2. W. Benz
3. Th. Henning
4. Y. Alibert
5. H. Klahr

Citations in the corpus

• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “The object around γ1 Leo A (HIP 50583) was found to have a projected mass of about 8.8 MX (Han et al. 2010).”