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 (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/570/A64
© ESO, 2014
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.