On the correlation of elemental abundances with kinematics among galactic disk stars

Mishenina, T. V.; Soubiran, C.; Kovtyukh, V. V.; Коротин, С. А.

doi:10.1051/0004-6361:20034454

Cited by 190 publications

(250 citation statements)

References 58 publications

(107 reference statements)

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“…This is because the thin disk and the thick disk within the Milky Way are discrete populations showing distinct chemical distributions in several elements, and in particular in α-elements. In fact, the Galactic thin and thick disks appear to overlap significantly around −0.7 < ∼ [Fe/H] < ∼ 0.0 dex when the iron abundance is used as a reference, while they are separated in [α/Fe] (see, e.g., Bensby et al 2003;Mishenina et al 2004). Here, we investigate to which population the XO-2 stellar system belongs to take advantage of 431 stars listed in the catalog by Soubiran & Girard (2005) and 906 FGK dwarf stars analyzed by Adibekyan et al (2012) with thin-disk, thick-disk, and halo membership probabilities (P thin , P thick , P halo ) higher than 90%.…”

Section: Stellar Population Of the Xo-2 Componentsmentioning

confidence: 99%

The GAPS programme with HARPS-N at TNG

Biazzo

Gratton

Desidera

et al. 2015

A&A

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Binary stars hosting exoplanets are a unique laboratory where chemical tagging can be performed to measure the elemental abundances of both stellar components with high accuracy, with the aim to investigate the formation of planets and their subsequent evolution. Here, we present a high-precision differential abundance analysis of the XO-2 wide stellar binary based on high-resolution HARPS-N at TNG spectra. Both components are very similar K-dwarfs and host planets. Since they formed presumably within the same molecular cloud, we expect that they possess the same initial elemental abundances. We investigated whether planets can cause some chemical imprints in the stellar atmospheric abundances. We measure abundances of 25 elements for both stars with a range of condensation temperature T C = 40−1741 K, achieving typical precisions of ∼0.07 dex. The northern component shows abundances in all elements higher by +0.067 ± 0.032 dex on average, with a mean difference of +0.078 dex for elements with T C > 800 K. The significance of the XO-2N abundance difference relative to XO-2S is at the 2σ level for almost all elements. We discuss that this result might be interpreted as the signature of the ingestion of material by XO-2N or depletion in XO-2S that is due to locking of heavy elements by the planetary companions. We estimate a mass of several tens of M ⊕ in heavy elements. The difference in abundances between XO-2N and XO-2S shows a positive correlation with the condensation temperatures of the elements, with a slope of (4.7 ± 0.9) × 10 −5 dex K −1 , which could mean that both components have not formed terrestrial planets, but first experienced the accretion of rocky core interior to the subsequent giant planets.

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Section: Stellar Population Of the Xo-2 Componentsmentioning

confidence: 99%

The GAPS programme with HARPS-N at TNG

Biazzo

Gratton

Desidera

et al. 2015

A&A

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“…Some stars from M08 were eliminated from the analysis because it was impossible to estimate the Li abundances owing to distortions of the spectra in the Li line region. A set of 24 stars was added with spectra that were previously analysed by Mishenina et al (2004) or retrieved from the ELODIE archive (Moultaka et al 2004). All 150 spectra were processed homogeneously using the same methods.…”

Section: Observations and The Spectral Processingmentioning

confidence: 99%

Activity and the Li abundances in the FGK dwarfs

Mishenina

Soubiran

Kovtyukh

et al. 2012

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Aims. The aim of the present study is to determine the Li abundances for a large set of the FGK dwarfs and to analyse the connections between the Li content, stellar parameters, and activity. Methods. The atmospheric parameters, rotational velocities and the Li abundances were determined from a homogeneous collection of the echelle spectra with high resolution and a high signal-to-noise ratio. The rotational velocities v sin i were determined by calibrating the cross-correlation function. The effective temperatures T eff were estimated by the line-depth ratio method. The surface gravities log g were computed by two methods: the iron ionization balance and the parallax. The LTE Li abundances were computed using synthetic spectra method. The behaviour of the Li abundance was examined in correlation with T eff , [Fe/H], as well as with v sin i and the level of activity in three stellar groups of the different temperature range. Results. The stellar parameters and the Li abundances are presented for 150 slow rotating stars of the lower part of the main sequence. The studied stars show a decline in the Li abundance with decreasing temperature T eff and a significant spread, which should be due to the difference of age of stars. The correlations between the Li abundances, rotational velocities v sin i, and the level of the chromospheric activity were discovered for the stars with 6000 > T eff > 5700 K, and it is tighter for the stars with 5700 > T eff > 5200 K. The target stars with T eff < 5200 K do not show any correlation between log A(Li) and v sin i. The relationship between the chromospheric and coronal fluxes in active with detected Li as well as in less active stars gives a hint that there exist different conditions in the action of the dynamo mechanism in those stars. Conclusions. We found that the Li-activity correlation is evident only in a restricted temperature range and the Li abundance spread seems to be present in a group of low chromospheric activity stars that also show a broad spread in the chromospheric vs. coronal activity.

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“…The atomic model of magnesium used in this work is essentially the same as the one described in Mishenina et al (2004).…”

Section: Magnesiummentioning

confidence: 99%

“…The detailed structure of the multiplets was ignored and each LS multiplet was considered as a single term. The fine structure was taken into account only for the 3s3p 3 P • level (more details in Mishenina et al 2004). …”

Section: Magnesiummentioning

confidence: 99%

Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

Andrievsky¹,

Spite²,

Коротин³

et al. 2010

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Aims. LTE abundances of light elements in extremely metal-poor (EMP) stars have been previously derived from high quality spectra. New derivations, free from the NLTE effects, will better constrain the models of the Galactic chemical evolution and the yields of the very first supernovae. Methods. The NLTE profiles of the magnesium and potassium lines have been computed in a sample of 53 extremely metal-poor stars with a modified version of the program MULTI and adjusted to the observed lines in order to derive the abundances of these elements. Results. The NLTE corrections for magnesium and potassium are in good agreement with the works found in the literature. The abundances are slightly changed, reaching a better precision: the scatter around the mean of the abundance ratios has decreased. Magnesium may be used with confidence as reference element. Together with previously determined NLTE abundances of sodium and aluminum, the new ratios are displayed, for comparison, along the theoretical trends proposed by some models of the chemical evolution of the Galaxy, using different models of supernovae.

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On the correlation of elemental abundances with kinematics among galactic disk stars

Cited by 190 publications

References 58 publications

The GAPS programme with HARPS-N at TNG

The GAPS programme with HARPS-N at TNG

Activity and the Li abundances in the FGK dwarfs

Non-LTE abundances of Mg and K in extremely metal-poor stars and the evolution of [O/Mg], [Na/Mg], [Al/Mg], and [K/Mg] in the Milky Way

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