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Title:
The HARPS search for southern extra-solar planets. XXVIII. Up to seven planets orbiting HD 10180: probing the architecture of low-mass planetary systems
Authors:
Lovis, C.; Ségransan, D.; Mayor, M.; Udry, S.; Benz, W.; Bertaux, J.-L.; Bouchy, F.; Correia, A. C. M.; Laskar, J.; Lo Curto, G.; Mordasini, C.; Pepe, F.; Queloz, D.; Santos, N. C.
Affiliation:
AA(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland ), AB(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland), AC(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland), AD(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland), AE(Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012, Bern, Switzerland), AF(Université Versailles Saint-Quentin, LATMOS-IPSL, 11 Boulevard d'Alembert, 78280, Guyancourt, France), AG(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis Bd Arago, 75014, Paris, France; Observatoire de Haute-Provence, CNRS/OAMP, 04870 St. Michel l', Observatoire, France), AH(Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal), AI(ASD, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Av. Denfert-Rochereau, 75014, Paris, France), AJ(European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748, Garching bei München, Germany), AK(Max-Planck-Institut für Astronomie, Königstuhl 17, 69117, Heidelberg, Germany; Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012, Bern, Switzerland), AL(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland), AM(Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland), AN(Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, 4150-762, Porto, Portugal; Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290, Versoix, Switzerland)
Publication:
Astronomy & Astrophysics, Volume 528, id.A112, 16 pp. (A&A Homepage)
Publication Date:
04/2011
Origin:
EDP Sciences
Astronomy Keywords:
planets and satellites: detection, stars: individual: HD 10180, techniques: radial velocities, techniques: spectroscopic
DOI:
10.1051/0004-6361/201015577
Bibliographic Code:
2011A&A...528A.112L

Abstract

Context. Low-mass extrasolar planets are presently being discovered at an increased pace by radial velocity and transit surveys, which opens a new window on planetary systems.
Aims: We are conducting a high-precision radial velocity survey with the HARPS spectrograph, which aims at characterizing the population of ice giants and super-Earths around nearby solar-type stars. This will lead to a better understanding of their formation and evolution, and will yield a global picture of planetary systems from gas giants down to telluric planets.
Methods: Progress has been possible in this field thanks in particular to the sub-m s-1 radial velocity precision achieved by HARPS. We present here new high-quality measurements from this instrument.
Results: We report the discovery of a planetary system comprising at least five Neptune-like planets with minimum masses ranging from 12 to 25 M⊕, orbiting the solar-type star HD 10180 at separations between 0.06 and 1.4 AU. A sixth radial velocity signal is present at a longer period, probably caused by a 65-M⊕ object. Moreover, another body with a minimum mass as low as 1.4 M⊕ may be present at 0.02 AU from the star. This is the most populated exoplanetary system known to date. The planets are in a dense but still well separated configuration, with significant secular interactions. Some of the orbital period ratios are fairly close to integer or half-integer values, but the system does not exhibit any mean-motion resonances. General relativity effects and tidal dissipation play an important role to stabilize the innermost planet and the system as a whole. Numerical integrations show long-term dynamical stability provided true masses are within a factor ~3 from minimum masses. We further note that several low-mass planetary systems exhibit a rather "packed" orbital architecture with little or no space left for additional planets. In several cases, semi-major axes are fairly regularly spaced on a logarithmic scale, giving rise to approximate Titius-Bode-like (i.e. exponential) laws. These dynamical architectures can be interpreted as the signature of formation scenarios where type I migration and interactions between protoplanets play a major role. However, it remains challenging to explain the presence of so many Neptunes and super-Earths on non-resonant, well-ordered orbits within ~1-2 AU of the central star. Finally, we also confirm the marked dependence of planet formation on both metallicity and stellar mass. Very massive systems are all found around metal-rich stars more massive than the Sun, while low-mass systems are only found around metal-deficient stars less massive than the Sun.

Based on observations made with the HARPS instrument on the ESO 3.6-m telescope at La Silla Observatory (Chile), under program IDs 072.C-0488 and 183.C-0972.Radial velocities are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/528/A112

Associated Articles

Part  1     Part  2     Part  3     Part  4     Part  6     Part  5     Part  7     Part  8     Part 11     Part  9     Part 10     Part 12     Part 13     Part 14     Part 15     Part 17     Part 18     Part 19     Part 20     Part 21     Part 22     Part 23     Part 24     Part 25     Part 26     Part 27     Part 28     Part 29     Part 30     Catalog Description     Part 31     Part 32     Part 33     Part 34     Part 35    

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