Volume 570, October 2014
|Number of page(s)||8|
|Section||Planets and planetary systems|
|Published online||17 October 2014|
1 N. Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland
2 Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele, Staffordshire, ST5 5BG, UK
3 Department of Physics, University of Warwick, Coventry CV4 7AL, UK
4 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
5 INAF – Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy
6 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife, KY16 9SS, UK
7 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Sart Tilman, Liège 1, Belgium
8 Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France
9 Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l’ Observatoire, France
10 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
11 Cavendish Laboratory, J J Thomson Avenue, Cambridge CB3 0HE, UK
12 Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
Received: 5 August 2014
Accepted: 9 September 2014
We have used the WASP survey to discover two exoplanetary systems, each consisting of a Jupiter-sized planet transiting an 11th-magnitude (V) main-sequence star. WASP-104b orbits its star in 1.75 d, whereas WASP-106b has the fourth-longest orbital period of any planet discovered by means of transits observed from the ground, orbiting every 9.29 d. Each planet is more massive than Jupiter (WASP-104b has a mass of 1.27 ± 0.05MJup, while WASP-106b has a mass of 1.93 ± 0.08MJup). Both planets are just slightly larger than Jupiter, with radii of 1.14 ± 0.04 and 1.09 ± 0.04RJup for WASP-104 and WASP-106, respectively. No significant orbital eccentricity is detected in either system, and while this is not surprising in the case of the short-period WASP-104b, it is interesting in the case of WASP-106b, because many otherwise similar planets are known to have eccentric orbits.
Key words: planets and satellites: detection / planets and satellites: fundamental parameters / stars: individual: WASP-104b / stars: individual: WASP-106b / planetary systems
Table 1 is available in electronic form at http://www.aanda.org
The table of photometry is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/570/A64
© ESO, 2014
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