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Eccentricity in Planetary Systems and the Role of Binarity C Eccentricity in planetary systems and the role of binarity C. Moutou, Arthur Vigan, D. Mesa, S. Desidera, P. Thebault, A. Zurlo, G. Salter To cite this version: C. Moutou, Arthur Vigan, D. Mesa, S. Desidera, P. Thebault, et al.. Eccentricity in planetary systems and the role of binarity: Sample definition, initial results, and the system of HD 211847. Astronomy and Astrophysics - A&A, EDP Sciences, 2017, 602, pp.A87. 10.1051/0004-6361/201630173. hal- 01678371 HAL Id: hal-01678371 https://hal.archives-ouvertes.fr/hal-01678371 Submitted on 16 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. A&A 602, A87 (2017) Astronomy DOI: 10.1051/0004-6361/201630173 & c ESO 2017 Astrophysics Eccentricity in planetary systems and the role of binarity Sample definition, initial results, and the system of HD 211847? C. Moutou1; 2, A. Vigan2, D. Mesa3, S. Desidera3, P. Thébault4, A. Zurlo5; 6, and G. Salter2 1 CNRS, CFHT, 65-1238 Mamalahoa Hwy, Kamuela HI 96743, USA e-mail: [email protected] 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 ABSTRACT 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 1. Introduction eccentricity and inclinations while tidal dissipation from the cen- tral star circularizes the orbit (Wu et al. 2007). For tighter bi- The distribution of eccentricities amongst the exoplanet pop- naries, it is the secular perturbations of the secondary that can ulation discovered by the radial-velocity method is intriguing, force high eccentricities on circumprimary planets (see for ex. as nearly circular orbits such as those in the solar system co- HD 41004 or HD 196885, Thebault 2011). exist with much more eccentric ones. Approximately 12% of Simulating the dynamical evolution of planetary systems re- these RV planets have eccentricities more than 0.5 and 45% quires the global knowledge of all components of the system and have eccentricities larger than 0.2, which is the maximum ec- the presence of a distant stellar companion is evidently a signif- centricity in the solar system (Mercury). Where planets mostly icant piece of information improving the accuracy of a model. formed via the core-accretion mechanism in the central part It is expected from theory that binaries with separations <50 au of circumstellar disks, little dynamical excitation is expected should have a strong impact on planet formation around the pri- (Pollack et al. 1996), and simulations of young planetary sys- mary (Thebault & Haghighipour 2014). However, observations tems have a clear tendency for coplanarity, circularity, and have revealed that some binaries as tight as 20 au indeed har- minimum energy exchange between planets. However, mod- bor planets (γ Cephei, HD 196885). Discovering new planet- els now exist for more excited systems implying planet-planet harboring tight binaries is therefore essential to our understand- scattering (Chatterjee et al. 2008), dynamical interactions with ing of how planet formation unfolds in such extreme conditions. a distant stellar companion, and/or the Kozai resonance mech- Unfortunately, the stellar multiplicity is generally not known at anism (Naoz et al. 2012; Wu et al. 2007; Kozai 1962). This the time of discovering a new planet with the RV method even Kozai mechanism involves the gravitational interaction between though it may seem trivial compared to the planet discovery: a planet and an outer stellar companion that is orbiting at large while equal-mass short-period binaries are discarded by imme- separations (up to several hundred au) from the central star. The diate spectroscopic analysis, long-period stellar companions are gravitational interactions between both objects induces Kozai more difficult to recognize since their signatures may take tens oscillations, which gradually pump the planetary orbit to high of years to reveal themselves. For instance, a 0.1 solar mass companion located on a 105-day orbit from a solar-type star ? Based on observations collected with SPHERE on the Very Large has a semi-amplitude of 60 m/s over 274 yr equivalent to non- Telescope (ESO, Chile). detectable trend over the typical 2–3 yr of RV monitoring. Such Article published by EDP Sciences A87, page 1 of 16 A&A 602, A87 (2017) the system to one sample or the other according to the eccentric- ity of the outermost planet, since it is the one most susceptible to the effect of massive companions at further distances. We have listed relevant parameters of systems in Tables1 and2 and their distribution in the planet mass-eccentricity diagram is shown in Fig.1. Errors on the parameters are not replicated in these ta- bles but can be found in the Exoplanet Encyclopedia1. Note that three additional systems were observed, HD 47186, HD 92788, and HD 168443, which were originally put in the comparison sample, but for which the outermost planet has intermediate ec- centricity and does not fulfill any of our criteria anymore (they were misclassified or updated). However, since they were ob- served their data has been included in the reduction and analysis. Their parameters are given in the bottom lines of Table2. The magnitude limit is set to allow the full sample to be Fig. 1. Eccentricity as a function of minimum companion mass of the observed in a short time as a bad-weather filler program using systems where these parameters are known (open circles), and of the VLT/SPHERE to either confirm or reject the presence of outer, sample of systems considered in this study (filled circles). massive companions, focusing on the closest separation range. It is interesting to note that the comparison sample con- tains much more multi-planet systems than the “eccentric sam- secondary components, however, would be located at 0.400 for a ple” (ten vs. four): this is, however, expected due to dynamical 100 pc distance system and would have a magnitude difference interactions (e.g., Lissauer et al. 2011) and/or detection biases of six in the H band, making them detectable in direct imaging in radial-velocity surveys. A similar observation was made by with instruments such as VLT/SPHERE (Beuzit et al. 2008) that Desidera & Barbieri(2007). provide high-contrast capabilities within one arcsecond. A literature search reveals that several of these planet hosts Determining any correlation between eccentric systems and are in multiple stellar systems. The compilation of known bi- the presence of distant massive companions would directly test nary (and one triple) systems is given in Table3. Their projected the formation/migration mechanisms. In addition, peculiar sys- distance ranges from 21 to 9100 au, with a median of ∼600 au. tems with detection of secondary components could be scruti- There are ten known multiple systems in the eccentric sample, nized with dedicated modeling, as done for α Cen or HD 196885 and three in the comparison sample. Seven of these systems have (Thébault et al. 2009; Thebault 2011). ∆K less than 2.0. Several imaging programs have observed exoplanet-hosting stars in the past. For instance, Mugrauer et al.(2014) and refer- ences therein presented SOFI imaging observations of such sys- 3. Observations and analysis tems; their observations probed the separations of 30 to 200 arc- 3.1. Instrument and strategy sec revealing that 13% of exoplanet host stars in their sample contained distant stellar companions. Narita et al.(2012) discov- We used the adaptive-optics instrument SPHERE at the Very ered the stellar companion to HAT-P-7 (with a magnitude dif- Large Telescope (ESO, Chile; Beuzit et al.
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