Spectroscopic metallicities for planet-host  stars: Extending 
 the samples

Santos, N. C.; Israelian, G.; Mayor, M.; Bento, J.; Almeida, Pedro Duarte de; Sousa, S. G.; Ecuvillon, A.

doi:10.1051/0004-6361:20052895

Cited by 223 publications

(274 citation statements)

References 36 publications

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“…This sample was presented as a comparison sample in Santos et al (2004), where the metallicities of all the stars were determined using a cross correlation function (CCF) calibration. We have already a spectroscopic determination for a significant number of stars within the CORALIE sample for which we derived precise spectroscopic parameters using HARPS spectra analysed in previous work for other different planet search samples (Santos et al 2004(Santos et al , 2005Sousa et al 2006Sousa et al , 2008Sousa et al , 2010. In Fig.…”

Section: [Fe/h] Based On the Ccf Calibrationmentioning

confidence: 99%

Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample

Sousa

Santos

Israelian

et al. 2011

A&A

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To understand the formation and evolution of solar-type stars and planets in the solar neighborhood, we need to obtain their stellar parameters with high precision. We present a catalog of precise stellar parameters for low-activity FGK single stars in a volumelimited sample followed by the HARPS spectrograph in the quest to identify extra-solar planets. The spectroscopic analysis was completed assuming LTE with a grid of Kurucz atmosphere models and using the ARES code to perform an automatic measurement of the line equivalent widths. The results are compared with different independent methods and also with other values found in the literature for common stars. Both comparisons are consistent and illustrate the homogeneity of the parameters derived by our team. The derived metallicities of this sample reveal a somewhat different distribution for the present planet hosts, but still indicates the already known higher frequency of planets observed for the more metal-rich stars. We combine the results derived in this sample with the one from the CORALIE survey to present the largest homogeneous spectroscopic study of the metallicity-giant-planet relation using a total of 1830 stars.

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Section: [Fe/h] Based On the Ccf Calibrationmentioning

confidence: 99%

Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample

Sousa

Santos

Israelian

et al. 2011

A&A

Self Cite

277

310

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“…The recent observation that (solar-like) stars with planets are on average more metal rich than similar stars without planets (e.g. Santos et al 2001Santos et al , 2004Santos et al , 2005Fischer et al 2003) is at least suggestive that this maybe also the case for binaries. Of particular interest is the fact that the Li abundance seem to differ between single stars and stars which host giant planets , and even between otherwise identical twin-star binaries (Martín et al 2002;Dall et al 2005), possibly related to pre-MS accretion of planetesimals or engulfment of planets.…”

Section: Introductionmentioning

confidence: 99%

Binarity, activity and metallicity among late-type stars

Dall¹,

Bruntt²,

Strassméier

2005

A&A

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We present the first in a series of papers that attempt to investigate the relation between binarity, magnetic activity, and chemical surface abundances of cool stars. In the current paper, we lay out and test two abundance analysis methods and apply them to two well-known, active, single stars, HD 27536 (G8IV-III) and HD 216803 (K5V), presenting photospheric fundamental parameters and abundances of Li, Al, Ca, Si, Sc, Ti, V, Cr, Fe, Co and Ni. The abundances from the two methods agree within the errors for all elements except calcium in HD 216803, which means that either method yields the same fundamental model parameters and the same abundances. Activity is described by the radiative loss in the Ca ii H and K lines with respect to the bolometric luminosity, through the activity index R HK . Binarity is established by very precise radial velocity (RV) measurements using HARPS spectra. The spectral line bisectors are examined for correlations between RV and bisector shape to distinguish between the effects of stellar activity and unseen companions. We show that HD 27536 exhibit RV variations mimicking the effect of a low-mass (m ∼ 4 M J ) companion in a relatively close (a ∼ 1 AU) orbit. The variation is strongly correlated with the activity, and consistent with the known photometric period P = 306.9 d, demonstrating a remarkable coherence between R HK and the bisector shape, i.e. between the photosphere and the chromosphere. We discuss the complications involved in distinguishing between companion and activity induced RV variations.

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“…The most significant finding in this area has been the observed strong correlation between stars' iron abundances 2) and the frequency of giant planets detected with the radial velocity method [114][115][116]. Iron is an important element because it traces a star's overall metal content (or metallicity) reasonably well and exhibits numerous lines in the optical spectra of solar-type stars that can be analyzed for determination of abundance.…”

Section: Planet-stellar Composition Correlationmentioning

confidence: 99%

Exoplanet Observations

Bean

2010

Formation and Evolution of Exoplanets

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Spectroscopic metallicities for planet-host stars: Extending the samples

Cited by 223 publications

References 36 publications

Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample

Spectroscopic stellar parameters for 582 FGK stars in the HARPS volume-limited sample

Binarity, activity and metallicity among late-type stars

Exoplanet Observations

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