The Chemical Composition of Field RR Lyrae Stars. I. Iron and Calcium

Lambert, David L.; Heath, James E.; Lemke, Michael; Drake, J. J.

doi:10.1086/192274

Cited by 173 publications

(222 citation statements)

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“…We found that the mean di †erence in log (gf ) is ]0.05^0.02 when comparing 68 lines in common between these latest works. Similar o †sets are found by Lambert et al (1996).…”

Section: The Veninsupporting

confidence: 81%

Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. II. Iron Abundance

Ramírez

Cohen

Buss

et al. 2001

The Astronomical Journal

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We present [Fe/H] abundance results that involve a sample of stars with a wide range in luminosity, from luminous giants to stars near the turno † in a globular cluster. Our sample of 25 stars in M71 includes 10 giant stars more luminous than the RHB, three horizontal branch stars, nine giant stars less luminous than the RHB, and three stars near the turno †. We analyzed both Fe I and Fe II lines in high-dispersion spectra observed with HIRES at the W. M. Keck Observatory. We Ðnd that the [Fe/H] abundances from both Fe I and Fe II lines agree with each other and with earlier determinations. Also the [Fe/H] obtained from Fe I and Fe II lines is constant within the rather small uncertainties for this group of stars over the full range in and luminosity, suggesting that non-LTE e †ects are negligible in T eff our iron abundance determination. In this globular cluster, there is no di †erence among the mean [Fe/H] of giant stars located at or above the RHB, RHB stars, giant stars located below the RHB and stars near the turno †.

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“…We found that the mean di †erence in log (gf ) is ]0.05^0.02 when comparing 68 lines in common between these latest works. Similar o †sets are found by Lambert et al (1996).…”

Section: The Veninsupporting

confidence: 81%

Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. II. Iron Abundance

Ramírez

Cohen

Buss

et al. 2001

The Astronomical Journal

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“…The latter were obtained by fitting Gaussian profiles to the observed ones. The log g f values for the Fe i and Fe ii lines were taken from Lambert et al (1996) and Castro et al (1997).…”

Section: Line Selection Measurements and Oscillator Strengthsmentioning

confidence: 99%

Chemical abundances and kinematics of a sample of metal-rich barium stars

Pereira

Silva

Chavero

et al. 2011

A&A

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Aims. We determined the atmospheric parameters and abundance pattern for a sample of metal-rich barium stars. Methods. We used high-resolution optical spectroscopy. Atmospheric parameters and abundances were determined using the local thermodynamic equilibrium atmosphere models of Kurucz and the spectral analysis code MOOG. Results. We show that the stars have enhancement factors, [s/Fe], from 0.25 to 1.16. Their abundance pattern of the Na, Al, α-elements, and iron group elements as well as their kinematical properties are similar to the characteristics of the other metal-rich and super metal-rich stars already analyzed. We conclude that metal-rich barium stars do not belong to the bulge population. We also show that metal-rich barium stars are useful targets for probing the s-process enrichment in high-metallicity environments.

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“…The iron lines taken from Lambert et al (1996) and Santos et al (2004) were carefully chosen by verifying that each line was not too strong, and checked for possible blending. We adopted new log g f values for the iron lines.…”

Section: Stellar Parameters and Iron Abundancesmentioning

confidence: 99%

Distribution of refractory and volatile elements in CoRoT exoplanet host stars

Chavero

Reza

Domingos³

et al. 2010

A&A

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The relative distribution of abundances of refractory, intermediate, and volatile elements in stars with planets can be an important tool for investigating the internal migration of a giant planet. This migration can lead to the accretion of planetesimals and the selective enrichment of the star with these elements. We report on a spectroscopic determination of the atmospheric parameters and chemical abundances of the parent stars in transiting planets . Adding data for CoRoT-3 and CoRoT-5 from the literature, we find a flat distribution of the relative abundances as a function of their condensation temperatures. For CoRoT-2, the relatively high lithium abundance and intensity of its Li i resonance line permit us to propose an age of 120 Myr, making this star one of the youngest stars with planets to date. We introduce a new methodology to investigate a relation between the abundances of these stars and the internal migration of their planets. By simulating the internal migration of a planet in a disk formed only by planetesimals, we are able, for the first time, to separate the stellar fractions of refractory, intermediate, and volatile rich planetesimals accreting onto the central star. Intermediate and volatile element fractions enriching the star are similar and much larger than those of pure refractory ones. This result is opposite to what has been considered in the literature for the accreting self-enrichment processes of stars with planets. We also show that these results are highly dependent on the model adopted for the disk distribution regions in terms of refractory, intermediate, and also volatile elements and other parameters considered. We note however, that this self-enrichment mechanism is only efficient during the first 20-30 Myr or later in the lifetime of the disk when the surface convection layers of the central star for the first time attain its minimum size configuration.

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The Chemical Composition of Field RR Lyrae Stars. I. Iron and Calcium

Cited by 173 publications

References 0 publications

Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. II. Iron Abundance

Abundances in Stars from the Red Giant Branch Tip to Near the Main-Sequence Turnoff in M71. II. Iron Abundance

Chemical abundances and kinematics of a sample of metal-rich barium stars

Distribution of refractory and volatile elements in CoRoT exoplanet host stars

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