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Lithium and Hα in stars and brown dwarfs of σ Orionis

Zapatero Osorio, M. R. and Béjar, V. J. S. and Pavlenko, Ya. and Rebolo, R. and Allende Prieto, C. and Martín, E. L. and García López, R. J. (2002) Lithium and Hα in stars and brown dwarfs of σ Orionis. Astronomy & Astrophysics, 384 (3). pp. 937-953. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20180214-090657976

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Abstract

We present intermediate- and low-resolution optical spectra around Hα and Li I λ6708 Å for a sample of 25 low mass stars and 2 brown dwarfs with confirmed membership in the pre-main sequence stellar σ Orionis cluster. Our observations are intended to investigate the age of the cluster. The spectral types derived for our target sample are found to be in the range K6–M8.5, which corresponds to a mass interval of roughly 1.2–0.02 M⊙ on the basis of state-of-the-art evolutionary models. Radial velocities (except for one object) are found to be consistent with membership in the Orion complex. All cluster members show considerable Hα emission and the Li I resonance doublet in absorption, which is typical of very young ages. We find that our pseudo-equivalent widths of Hα and Li I (measured relative to the observed local pseudo-continuum formed by molecular absorptions) appear rather dispersed (and intense in the case of Hα) for objects cooler than M3.5 spectral class, occurring at the approximate mass where low mass stars are expected to become fully convective. The least massive brown dwarf in our sample, S Ori 45 (M8.5, ~0.02 M⊙), displays variable Hα emission and a radial velocity that differs from the cluster mean velocity. Tentative detection of forbidden lines in emission indicates that this brown dwarf may be accreting mass from a surrounding disk. We also present recent computations of Li  I λ6708 Å curves of growth for low gravities and for the temperature interval (about 4000–2600 K) of our sample. The comparison of our observations to these computations allows us to infer that no lithium depletion has yet taken place in σ Orionis, and that the observed pseudo-equivalent widths are consistent with a cluster initial lithium abundance close to the cosmic value. Hence, the upper limit to the σ Orionis cluster age can be set at 8 Myr, with a most likely value around 2–4 Myr.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361:20020046DOIArticle
https://www.aanda.org/articles/aa/abs/2002/12/aa1839/aa1839.htmlPublisherArticle
https://arxiv.org/abs/astro-ph/0202147arXivDiscussion Paper
ORCID:
AuthorORCID
Rebolo, R.0000-0003-3767-7085
Allende Prieto, C.0000-0002-0084-572X
Alternate Title:Lithium and Halpha in stars and brown dwarfs of sigma Orionis
Additional Information:© 2002 ESO. Article published by EDP Sciences. Received 24 August 2001; Accepted 2 January 2002; Published online 15 March 2002. Based on observations made with the following telescopes: 3.5-m telescope at the Spanish-German Calar Alto Observatory (Spain) operated by the Max-Planck-Institut für Astronomie in Heidelberg (Germany); 2.5-m Isaac Newton telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias; 2.1-m Otto Struve telescope at McDonald Observatory (USA); and the 10-m Keck II telescope of the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (the Observatory was made possible by the generous financial support of the W. M. Keck Foundation). We are grateful to I. Baraffe and colleagues for making electronic files of their evolutionary models available to us, and to Louise Good for correcting the English language used in the manuscript. We also thank the staff at McDonald Observatory, especially David Doss, for their helpful assistance. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Partial financial support was provided by the Spanish DGES PB98-0531-C02-02. YP acknowledges partial financial support from Small Research Grant of American Astronomical Society. CAP acknowledges partial financial support from NSF (AST-0086321).
Funders:
Funding AgencyGrant Number
Direção-Geral do Ensino Superior (DGES)PB98-0531-C02-02
American Astronomical SocietyUNSPECIFIED
NSFAST-0086321
Subject Keywords:circumstellar matter - stars: abundances - stars: late-type - stars: low mass, brown dwarfs - stars: pre-main sequence - open clusters and associations: σ Orionis
Issue or Number:3
Record Number:CaltechAUTHORS:20180214-090657976
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180214-090657976
Official Citation:Lithium and Hα in stars and brown dwarfs of σ Orionis M. R. Zapatero Osorio, V. J. S. Béjar, Ya. Pavlenko, R. Rebolo, C. Allende Prieto, E. L. Martín and R. J. García López A&A, 384 3 (2002) 937-953. DOI: https://doi.org/10.1051/0004-6361:20020046
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:84826
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:15 Feb 2018 00:17
Last Modified:09 Mar 2020 13:19

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