Volume 548, December 2012
|Number of page(s)||7|
|Section||Planets and planetary systems|
|Published online||03 December 2012|
Detection of an exoplanet around the evolved K giant HD 66141
1 Korea Astronomy and Space Science Institute, 776, Daedeokdae-Ro, Youseong-Gu, 305-348 Daejeon, Korea
e-mail: firstname.lastname@example.org; email@example.com; firstname.lastname@example.org
2 National Astronomical Research Institute of Thailand, 50200 Chiang Mai, Thailand
3 Crimean Astrophysical Observatory, Nauchny, 98409 Crimea, Ukraine
4 Department of Astronomy and Atmospheric Sciences, Kyungpook National University, 702-701 Daegu, Korea
Received: 5 September 2011
Accepted: 6 November 2012
Aims. We have been carrying out a precise radial velocity (RV) survey for K giants to search for and study the origin of the low-amplitude and long-periodic RV variations.
Methods. We present high-resolution RV measurements of the K2 giant HD 66141 from December 2003 to January 2011 using the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at the Bohyunsan Optical Astronomy Observatory (BOAO).
Results. We find that the RV measurements for HD 66141 exhibit a periodic variation of 480.5 ± 0.5 days with a semi-amplitude of 146.2 ± 2.7 m s-1. The Hipparcos photometry and bisector velocity span (BVS) do not show any obvious correlations with RV variations. We find indeed 706.4 ± 35.0 day variations in equivalent width (EW) measurements of Hα line and 703.0 ± 39.4 day variations in a space-born measurements 1.25μ flux of HD 66141 measured during the COBE/DIRBE experiment. We reveal that a mean value of long-period variations is about 705 ± 53 days, whose origin is a rotation period of the star and variability that is caused by surface inhomogeneities. For the 480-day periods of RV variations an orbital motion is the most likely explanation. Assuming a stellar mass of 1.1 ± 0.1 M⊙ for HD 66141, we obtain a minimum mass for the planetary companion of 6.0 ± 0.3 MJup with an orbital semi-major axis of 1.2 ± 0.1 AU and an eccentricity of 0.07 ± 0.03.
Key words: planetary systems / stars: individual: HD 66141 / techniques: radial velocities
© ESO, 2012
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