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Title:
Planetary companions in K giants beta Cancri, mu Leonis, and beta Ursae Minoris
Authors:
Lee, B.-C.; Han, I.; Park, M.-G.; Mkrtichian, D. E.; Hatzes, A. P.; Kim, K.-M.
Affiliation:
AA(Korea Astronomy and Space Science Institute, 776, Daedeokdae-Ro, Youseong-Gu, 305-348, Daejeon, Korea ), AB(Korea Astronomy and Space Science Institute, 776, Daedeokdae-Ro, Youseong-Gu, 305-348, Daejeon, Korea ), AC(Department of Astronomy and Atmospheric Sciences, Kyungpook National University, 702-701, Daegu, Korea ), AD(National Astronomical Research Institute of Thailand, 50200, Chiang Mai, Thailand; Crimean Astrophysical Observatory, Taras Shevchenko National University of Kyiv, Nauchny, 98409, Crimea, Ukraine ), AE(Thüringer Landessternwarte Tautenburg (TLS), Sternwarte 5, 07778, Tautenburg, Germany ), AF(Korea Astronomy and Space Science Institute, 776, Daedeokdae-Ro, Youseong-Gu, 305-348, Daejeon, Korea )
Publication:
Astronomy & Astrophysics, Volume 566, id.A67, 7 pp. (A&A Homepage)
Publication Date:
06/2014
Origin:
EDP Sciences
Astronomy Keywords:
instrumentation: spectrographs, techniques: radial velocities, planetary systems
DOI:
10.1051/0004-6361/201322608
Bibliographic Code:
2014A&A...566A..67L

Abstract


Aims: The aim of our paper is to investigate the low-amplitude and long-period variations in evolved stars with a precise radial velocity survey.
Methods: The high-resolution, the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) was used from 2003 to 2013 for a radial velocity survey of giant stars as part of the exoplanet search program at Bohyunsan Optical Astronomy Observatory (BOAO).
Results: We report the detection of three new planetary companions orbiting the K giants beta Cnc, mu Leo, and beta UMi. The planetary nature of the radial velocity variations is supported by analyzes of ancillary data. The Hipparcos photometry shows no variations with periods close to those in radial velocity variations and there is no strong correlation between the bisector velocity span (BVS) and the radial velocities for each star. Furthermore, the stars show weak or no core reversal in Ca II H lines indicating that they are inactive stars. The companion to beta Cnc has a minimum mass of 7.8 MJup in a 605-day orbit with an eccentricity of 0.08. The giant mu Leo is orbited by a companion of minimum mass of 2.4 MJup having a period of 357 days and an eccentricity of 0.09. The giant beta UMi is a known barium star and is suspected of harboring a white dwarf or substellar mass companion. Its companion has a minimum mass of 6.1 MJup, a period of 522 days, and an eccentricity e = 0.19.

Based on observations made with the BOES instrument on the 1.8 m telescope at Bohyunsan Optical Astronomy Observatory in Korea.Tables 4-6 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/566/A67

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