This article has an erratum: [https://doi.org/10.1051/0004-6361/200810241e]
Volume 491, Number 3, December I 2008
|Page(s)||883 - 888|
|Section||Planets and planetary systems|
|Published online||03 October 2008|
V. A planetary system found with HARPS around the F6IV–V star HD 60532
Laboratoire d'Astrophysique de Grenoble, UMR 5571 CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France e-mail: email@example.com
2 Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
3 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
Accepted: 22 September 2008
Aims. In the framework of the search for extrasolar planets and brown dwarfs around early-type stars, we present the results obtained for the F-type main-sequence star HD 60532 (F6V) with HARPS.
Methods. Using 147 spectra obtained with HARPS at La Silla on a time baseline of two years, we studied the radial velocities of this star.
Results. HD 60532 radial velocities are periodically variable, and the variations have a Keplerian origin. This star is surrounded by a planetary system of two planets with minimum masses of 1 and 2.5 MJup and orbital separations of 0.76 and 1.58 AU, respectively. We also detect high-frequency, small-amplitude (10 m s-1 peak-to-peak) pulsations. Dynamical studies of the system point toward a possible 3:1 mean-motion resonance that should be confirmed within the next decade.
Key words: techniques: radial velocities / stars: early-type / stars: planetary systems / stars: individual: HD 60532 / stars: oscillations
Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, ESO. Program IDs 072.C-0488, 076.C-0279, 077.C-0295, 078.C-0209, 080.C-0664, 080.C-0712, 081.C-0774.
© ESO, 2008
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