EDP Sciences
Free access
Issue A&A
Volume 461, Number 1, January I 2007
Page(s) 171 - 182
Section Galactic structure, stellar clusters, and populations
DOI http://dx.doi.org/10.1051/0004-6361:20065872

A&A 461, 171-182 (2007)
DOI: 10.1051/0004-6361:20065872

Kinematics of planet-host stars and their relation to dynamical streams in the solar neighbourhood

A. Ecuvillon1, G. Israelian1, F.  Pont2, N. C. Santos2, 3, 4, and M. Mayor2

1  Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
    e-mail: aecuvill@ll.iac.es
2  Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
3  Centro de Astronomia e Astrofisica de Universidade de Lisboa, Observatorio Astronomico de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal
4  Centro de Geofisica de Évora, Rua Romaõ Ramalho 59, 7000 Évora, Portugal

(Received 21 June 2006 / Accepted 28 August 2006)

We present a detailed study on the kinematics of metal-rich stars with and without planets, and their relation to the Hyades, Sirius and Hercules dynamical streams in the solar neighbourhood. Accurate kinematics have been derived for all the stars belonging to the CORALIE planet search survey. We used precise radial velocity measurements and CCF parameters from the CORALIE database, and parallaxes, photometry and proper motions from the HIPPARCOS and Tycho-2 catalogues. The location of stars with planets in the thin or thick discs has been analysed using both kinematic and chemical constraints. We compare the kinematic behaviour of known planet-host stars to the remaining targets belonging to the volume-limited sample, in particular to its metal-rich population. The high average metallicity of the Hyades stream is confirmed. The planet-host targets show a kinematic behaviour similar to that of the metal-rich comparison subsample, rather than to that of the comparison sample as a whole, thus supporting a primordial origin for the metal excess observed in stars with known planetary companions. According to the scenarios proposed as an explanation for the dynamical streams, systems with giant planets could have formed more easily in metal-rich inner Galactic regions and then been brought into the solar neighbourhood by dynamical streams.

Key words: planetary systems -- solar neighbourhood -- stars: kinematics -- stars: abundances -- Galaxy: kinematics and dynamics

© ESO 2006

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Editor-in-Chief: T. Forveille
Letters Editor-in-Chief: J. Alves
Managing Editor: C. Bertout

ISSN: 0004-6361 ; e-ISSN: 1432-0746
Frequency: 12 volumes per year
Published by: EDP Sciences

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