Lithium depletion in solar-like stars: no planet connection

Baumann, Patrick; Ramírez, Iván; Meléndez, Jorge; Asplund, Martin; Lind, Karin

doi:10.1051/0004-6361/201015137

Cited by 167 publications

(203 citation statements)

References 55 publications

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“…The ratio of stars with lithium to stars without detectable lithium is 8/3 = 2.6, which could reflect the fact that stars with lower log g are younger. Lithium depletion as a function of the age of stars is discussed by Baumann et al (2010) and Carlos et al (2016). On the other hand, we might expect to see the effects of increased shearing in a deeper convective envelope here.…”

Section: Discussionmentioning

confidence: 74%

“…Luck & Heiter (2006) found no differences between the lithium abundances of stars with and without planets. Baumann et al (2010) showed that for solar-like stars there are no statistical correspondence between the lithium abundances and age for stars with and without planets. Thus, the lithium abundance in stellar atmospheres is not affected by the presence of a planet near to a star.…”

Section: Introductionmentioning

confidence: 99%

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A detailed study of lithium in 107 CHEPS dwarf stars

Pavlenko

Jenkins

Ivanyuk

et al. 2018

A&A

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Context. We report results from lithium abundance determinations using high resolution spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire Extrasolar Planet Search programme. Aims. We aim to set out to understand the lithium distribution of the population of stars taken from this survey. Methods. The lithium abundance taking account of non-local thermodynamical equilibrium effects was determined from the fits to the Li I 6708 Å resonance doublet profiles in the observed spectra. Results. We find that a) fast rotators tend to have higher lithium abundances; b) log N(Li) is higher in more massive and hot stars; c) log N(Li) is higher in stars of lower log g; d) stars with the metallicities >0.25 dex do not show the lithium lines in their spectra; e) most of our planet hosts rotate slower; and f) a lower limit of lithium isotopic ratio is 7 Li/ 6 Li > 10 in the atmospheres of two stars with planets (SWP) and two non-SWP stars. Conclusions. Measurable lithium abundances were found in the atmospheres of 45 stars located at distances of 20−170 pc from the Sun, for the other 62 stars the upper limits of log N(Li) were computed. We found well defined dependences of lithium abundances on T eff , V sin i, and less pronounced for the log g. In case of V sin i we see two sequences of stars: with measurable lithium and with the upper limit of log N(Li). About 10% of our targets are known to host planets. Only two SWP have notable lithium abundances, so we found a lower proportion of stars with detectable Li among known planet hosts than among stars without planets. However, given the small sample size of our planet-host sample, our analysis does not show any statistically significant differences in the lithium abundance between SWP and stars without known planets.

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Section: Discussionmentioning

confidence: 74%

Section: Introductionmentioning

confidence: 99%

A detailed study of lithium in 107 CHEPS dwarf stars

Pavlenko

Jenkins

Ivanyuk

et al. 2018

A&A

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“…Adibekyan et al 2012a) with some curious trends being a strong matter of debate concerning e.g. the abundances of the light element lithium (Israelian et al 2009;Baumann et al 2010;Sousa et al 2010;Ghezzi et al 2010b) or specific trends including other elemental abundances (e.g. Ramírez et al 2010;González Hernández et al 2010).…”

Section: Introductionmentioning

confidence: 99%

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

A&A

286

255

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Context. Thanks to the importance that the star-planet relation has to our understanding of the planet formation process, the precise determination of stellar parameters for the ever increasing number of discovered extra-solar planets is of great relevance. Furthermore, precise stellar parameters are needed to fully characterize the planet properties. It is thus important to continue the efforts to determine, in the most uniform way possible, the parameters for stars with planets as new discoveries are announced. Aims. In this paper we present new precise atmospheric parameters for a sample of 48 stars with planets. We then take the opportunity to present a new catalogue of stellar parameters for FGK and M stars with planets detected by radial velocity, transit, and astrometry programs. Methods. Stellar atmospheric parameters and masses for the 48 stars were derived assuming local thermodynamic equilibrium (LTE) and using high-resolution and high signal-to-noise spectra. The methodology used is based on the measurement of equivalent widths for a list of iron lines and making use of iron ionization and excitation equilibrium principles. For the catalogue, and whenever possible, we used parameters derived in previous works published by our team, using well-defined methodologies for the derivation of stellar atmospheric parameters. This set of parameters amounts to over 65% of all planet host stars known, including more than 90% of all stars with planets discovered through radial velocity surveys. For the remaining targets, stellar parameters were collected from the literature. Results. The stellar parameters for the 48 stars are presented and compared with previously determined literature values. For the catalogue, we compile values for the effective temperature, surface gravity, metallicity, and stellar mass for almost all the planet host stars listed in the Extrasolar Planets Encyclopaedia. This data will be updated on a continuous basis. The compiled catalogue is available online. The data can be used for statistical studies of the star-planet correlation, as well as for the derivation of consistent properties for known planets.

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“…M67 is relatively nearby (∼900 pc) and is only little affected by interstellar extinction, which allows detailed spectroscopic studies of its main-sequence stars. The depleted Li abundance of the Sun seems rather representative of solar-twins in the Galactic field (Baumann et al 2010). M67 also seems to contain Li-depleted G stars (Pasquini et al 1997).…”

Section: Introductionmentioning

confidence: 99%

M67-1194, an unusually Sun-like solar twin in M67

Önehag

Korn

Gustafsson

et al. 2011

A&A

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Context. The rich open cluster M67 is known to have a chemical composition close to solar, and an age around 4 Gyr. It thus offers the opportunity to check our understanding of the physics and the evolution of solar-type stars in a cluster environment. Aims. We present the first spectroscopic study at high resolution, R ≈ 50 000, of the potentially best solar twin, M67-1194, identified among solar-like stars in M67. Methods. G dwarfs in M67 (d ≈ 900 pc) are relatively faint (V ≈ 15), which makes detailed spectroscopic studies time-consuming. Based on a pre-selection of solar-twin candidates performed at medium resolution by Pasquini et al. (2008, A&A, 489, 677), we explore the chemical-abundance similarities and differences between M67-1194 and the Sun, using VLT/FLAMES-UVES. Working with a solar twin in the framework of a differential analysis, we minimize systematic model errors in the abundance analysis compared to previous studies which utilized more evolved stars to determine the metallicity of M67. The differential approach yields precise and accurate chemical abundances for M67, which enhances the possibility to use this object in studies of the potential peculiarity, or normality, of the Sun. Results. We find M67-1194 to have stellar parameters indistinguishable from the solar values, with the exception of the overall metallicity which is slightly super-solar ([Fe/H] = 0.023 ± 0.015). An age determination based on evolutionary tracks yields 4.2 ± 1.6 Gyr. Most surprisingly, we find the chemical abundance pattern to closely resemble the solar one, in contrast to most known solar twins in the solar neighbourhood. Conclusions. We confirm the solar-twin nature of M67-1194, the first solar twin known to belong to a stellar association. This fact allows us to put some constraints on the physical reasons for the seemingly systematic departure of M67-1194 and the Sun from most known solar twins regarding chemical composition. We find that radiative dust cleansing by nearby luminous stars may be the explanation for the peculiar composition of both the Sun and M67-1194, but alternative explanations are also possible. The chemical similarity between the Sun and M67-1194 also suggests that the Sun once formed in a cluster like M67.

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Lithium depletion in solar-like stars: no planet connection

Cited by 167 publications

References 55 publications

A detailed study of lithium in 107 CHEPS dwarf stars

A detailed study of lithium in 107 CHEPS dwarf stars

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

M67-1194, an unusually Sun-like solar twin in M67

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