| Issue |
A&A
Volume 415, Number 3, March I 2004
|
|
|---|---|---|
| Page(s) | 1153 - 1166 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361:20034469 | |
| Published online | 13 February 2004 | |
Spectroscopic [Fe/H] for 98 extra-solar planet-host stars*
Exploring the probability of planet formation
1
Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
2
Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
3
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
Corresponding author: N. C. Santos, Nuno.Santos@oal.ul.pt
Received:
8
October
2003
Accepted:
4
November
2003
We present stellar parameters and metallicities,
obtained from a detailed spectroscopic analysis, for a large sample
of 98 stars known to be orbited by planetary mass companions
(almost all known targets), as well as for
a volume-limited sample of 41 stars not known to host any planet.
For most of the stars the stellar parameters are revised versions
of the ones presented in our previous work. However, we also present
parameters for 18 stars with planets not previously published,
and a compilation of stellar parameters for the remaining 4 planet-hosts
for which we could not obtain a spectrum.
A comparison of our stellar parameters with values of 
, 
, and [Fe/H] available in the literature
shows a remarkable agreement. In particular, our spectroscopic
values are now very close to trigonometric estimates
based on Hipparcos parallaxes.
The derived [Fe/H] values are then used to confirm the previously
known result that planets are more prevalent
around metal-rich stars. Furthermore, we confirm that the frequency of
planets is a strongly rising function
of the stellar metallicity, at least for stars with [Fe/H] > 0. While only about 3% of
the solar metallicity stars in the CORALIE planet search sample
were found to be orbited by a planet, this number increases to more
than 25% for stars with [Fe/H] above +0.3. Curiously, our results
also suggest that these percentages might
remain relatively constant for values of [Fe/H] lower than about
solar, increasing then linearly with the mass fraction of heavy elements.
These results are discussed in the context of the theories of planetary
formation.
Key words: stars: abundances / stars: fundamental parameters / stars: planetary systems / stars: planetary systems: formation / stars: chemically peculiar
Based on observations collected at the La Silla Observatory, ESO (Chile), with the CORALIE spectrograph at the 1.2-m Euler Swiss telescope and the FEROS spectrograph at the 1.52-m and 2.2-m ESO telescopes, with the VLT/UT2 Kueyen telescope (Paranal Observatory, ESO, Chile) using the UVES spectrograph (Observing run 67.C-0206, in service mode), with the TNG and William Herschel Telescopes, both operated at the island of La Palma, and with the ELODIE spectrograph at the 1.93-m telescope at the Observatoire de Haute Provence.
© ESO, 2004
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