The metal-rich nature of stars with planets

Santos, N. C.; Israelian, G.; Mayor, M.

doi:10.1051/0004-6361:20010648

Cited by 444 publications

(596 citation statements)

References 43 publications

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“…Based on large planetary surveys this correlation is well established by independent teams (Santos, Israelian & Mayor 2001, 2004aFischer & Valenti 2005). We have a completely different result if we examine the metallicity of host stars for systems having all planets less massive than 40 M ⊕ .…”

Section: The Correlation With the Metallicity Of Host Starsmentioning

confidence: 86%

The road to Earth twins – Karl Schwarzschild Award Lecture 2010

et al. 2011

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A rich population of low-mass planets orbiting solar-type stars on tight orbits has been detected by Doppler spectroscopy. These planets have masses in the domain of super-Earths and Neptune-type objects, and periods less than 100 days. In numerous cases these planets are part of very compact multiplanetary systems. Up to seven planets have been discovered orbiting one single star. These low-mass planets have been detected by the HARPS spectrograph around 30 % of solartype stars. This very high occurrence rate has been recently confirmed by the results of the Kepler planetary transit space mission. The large number of planets of this kind allows us to attempt a first characterization of their statistical properties, which in turn represent constraints to understand the formation process of these systems. The achieved progress in the sensitivity and stability of spectrographs have already led to the discovery of planets with masses as small as 1.5 M⊕.

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Section: The Correlation With the Metallicity Of Host Starsmentioning

confidence: 86%

The road to Earth twins – Karl Schwarzschild Award Lecture 2010

et al. 2011

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“…It is a K5 dwarf with a rotation period of 10.3 days but with a small projected rotational velocity of 2.6 km s −1 (Vogt et al 1983), indicating an inclination of approximately 30 • . The star has been studied recently by Santos et al (2001), who found atmospheric parameters and metallicity and placed it in a sample of comparison stars without planets.…”

Section: The Target Starsmentioning

confidence: 99%

“…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: 98%

Binarity, activity and metallicity among late-type stars

Dall¹,

Bruntt²,

Strassméier

2005

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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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“…Santos et al 2000Santos et al , 2001Santos et al , 2004Laws et al 2003;Fischer & Valenti 2005). Gradually, similar abundance studies were made for elements other than iron (e.g.…”

Section: Introductionmentioning

confidence: 99%

Chemical abundances of 451 stars from the HARPS GTO planet search program

Neves

Santos

Sousa

et al. 2009

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We present a uniform study of the chemical abundances of 12 elements (Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Na, Mg, and Al) derived from the spectra of 451 stars observed as part of one of the HARPS GTO planet search programs. Sixty eight of these are planetbearing stars. The main goals of our work are: i) the investigation of possible differences between the abundances of stars with and without planets; ii) the study of the possible differences in the abundances of stars in the thin and the thick disc. We confirm that there is a systematically higher metallicity in planet host stars, when compared to non planet-hosts, common to all studied species. We also found that there is no difference in the galactic chemical evolution trends of the stars with and without planets. Stars that harbour planetary companions simply appear to be in the high metallicity tail of the distribution. We also confirm that Neptunian and super-Earth class planets may be easier to find at lower metallicities. A statistically significative abundance difference between stars of the thin and the thick disc was found for [Fe/H] < 0. However, the populations from the thick and the thin disc cannot be clearly separated.

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The metal-rich nature of stars with planets

Cited by 444 publications

References 43 publications

The road to Earth twins – Karl Schwarzschild Award Lecture 2010

The road to Earth twins – Karl Schwarzschild Award Lecture 2010

Binarity, activity and metallicity among late-type stars

Chemical abundances of 451 stars from the HARPS GTO planet search program

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