Volume 415, Number 1, February III 2004
|Page(s)||391 - 402|
|Section||Planets and planetary systems|
|Published online||03 February 2004|
XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE
Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
2 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
Corresponding author: M. Mayor, firstname.lastname@example.org
Accepted: 25 September 2003
This paper summarizes the information gathered for 16 still unpublished exoplanet candidates discovered with the CORALIE echelle spectrograph mounted on the Euler Swiss telescope at La Silla Observatory. Amongst these new candidates, 10 are typical extrasolar Jupiter-like planets on intermediate- or long-period (100 < P ≤ 1350 d) and fairly eccentric (0.2 ≤ e ≤ 0.5) orbits (HD 19994, HD 65216, HD 92788, HD 111232, HD 114386, HD 142415, HD 147513, HD 196050, HD 216437, HD 216770). Two of these stars are in binary systems. The next 3 candidates are shorter-period planets (HD 6434, HD 121504) with lower eccentricities among which we find a hot Jupiter (HD 83443). More interesting cases are given by the multiple-planet systems HD 82943 and HD 169830. The former is a resonant = 2/1 system in which planet-planet interactions are influencing the system evolution. The latter is more hierarchically structured.
Key words: techniques: radial velocities / techniques: spectroscopic – stars: activity – stars: planetary systems
Based on observations collected with the CORALIE echelle spectrograph on the 1.2-m Euler Swiss telescope at La Silla Observatory, ESO Chile.
The precise radial velocities presented in this paper are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/415/391, except for the multi-planet systems that will appear in a future paper describing their dynamical evolutions, taking planet-planet interaction into account.
© ESO, 2004
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