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LITHIUM IN THE STELLAR OPEN CLUSTER M67

B. L. CANTO MARTINS

Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, 59072-970, Brazil

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J. D. DO NASCIMENTO, Jr.

Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, 59072-970, Brazil

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J. R. DE MEDEIROS

Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, 59072-970, Brazil

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A. LÈBRE

Groupe de Recherche en Astronomie et Astrophysique du Languedoc – UMR 5024/ISTEEM, (CNRS), Université Montpellier II, Place E. Bataillon, Montpellier, 34095, France

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O. RICHARD

Groupe de Recherche en Astronomie et Astrophysique du Languedoc – UMR 5024/ISTEEM, (CNRS), Université Montpellier II, Place E. Bataillon, Montpellier, 34095, France

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P. DE LAVERNY

Département Cassiopée – UMR 6202 (CNRS), Observatoire de la Côte d'Azur, BP 4229 Nice, 06304, France

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, and

C. MELO

European Southern Observatory and Departamento de Astronomìa, Universidad de Chile, Casilla Postal 36D, Santiago de Chile, Chile

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https://doi.org/10.1142/S021827180701016XCited by:1 (Source: Crossref)

Abstract

In this work we present atmospheric parameters and Li abundances, obtained from a detailed spectroscopic analysis, for a large sample of stars with different evolutionary stages (turn-off, subgiant and giant stars) in the open cluster M67. The observations were carried out with high resolution (R ~ 47,000) and high S/N using the UVES+FLAMES at VLT/UT2. From available photometry and computed synthetic spectra for the region around the lithium line at 6707.75 Å, we derive atmospheric parameters (T_eff, log g, [Fe/H], v sin i) and Li abundances for each star, in order to better understand the level of mixing and convective dilution of evolved stars in M67.

Based on observations collected at ESO, Paranal, Chile (VLT/FLAMES program ID 072.D-0309 and 074.D-0179).

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