Volume 602, June 2017
|Number of page(s)||16|
|Section||Planets and planetary systems|
|Published online||20 June 2017|
Eccentricity in planetary systems and the role of binarity
Sample definition, initial results, and the system of HD 211847⋆
1 CNRS, CFHT, 65-1238 Mamalahoa Hwy, Kamuela HI 96743, USA
2 Aix Marseille Univ., CNRS, LAM, Laboratoire d’Astrophysique de Marseille, 13284 Marseille, France
3 INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
4 LESIA, CNRS, Observatoire de Paris, Université Paris Diderot, UPMC, 5 place J. Janssen, 92190 Meudon, France
5 Nucleo de Astronoma, Facultad de Ingeniera, Univ. D. Portales, Av. Ejercito 441, 1515 Santiago, Chile
6 Universidad de Chile, Camino del Observatorio, 1515 Santiago, Chile
Received: 1 December 2016
Accepted: 17 December 2016
We explore the multiplicity of exoplanet host stars with high-resolution images obtained with VLT/SPHERE. Two different samples of systems were observed: one containing low-eccentricity outer planets, and the other containing high-eccentricity outer planets. We find that 10 out of 34 stars in the high-eccentricity systems are members of a binary, while the proportion is 3 out of 27 for circular systems. Eccentric-exoplanet hosts are, therefore, significantly more likely to have a stellar companion than circular-exoplanet hosts. The median magnitude contrast over the 68 data sets is 11.26 and 9.25, in H and K, respectively, at 0.30 arcsec. The derived detection limits reveal that binaries with separations of less than 50 au are rarer for exoplanet hosts than for field stars. Our results also imply that the majority of high-eccentricity planets are not embedded in multiple stellar systems (24 out of 34), since our detection limits exclude the presence of a stellar companion. We detect the low-mass stellar companions of HD 7449 and HD 211847, both members of our high-eccentricity sample. HD 7449B was already detected and our independent observation is in agreement with this earlier work. HD 211847’s substellar companion, previously detected by the radial velocity method, is actually a low-mass star seen face-on. The role of stellar multiplicity in shaping planetary systems is confirmed by this work, although it does not appear as the only source of dynamical excitation.
Key words: binaries: visual / techniques: high angular resolution / planetary systems
© ESO, 2017
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