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Sulfur Abundances in Orion B Stars

Published online by Cambridge University Press:  09 March 2010

Simone Daflon ,
Katia Cunha ,
Ramiro de la Reza ,
Jon Holtzman  and
Cristina Chiappini
Simone Daflon
Affiliation:
Observatório Nacional, Rua General José Cristino 77, CEP 20921-400, Rio de Janeiro, Brazil email:daflon@on.br
Katia Cunha
Affiliation:
Observatório Nacional, Rua General José Cristino 77, CEP 20921-400, Rio de Janeiro, Brazil email:daflon@on.br National Optical Astronomy Observatories, 950 N. Cherry Ave., Tucson, AZ 85719
Ramiro de la Reza
Affiliation:
Observatório Nacional, Rua General José Cristino 77, CEP 20921-400, Rio de Janeiro, Brazil email:daflon@on.br
Jon Holtzman
Affiliation:
New Mexico State University, 1320 Frenger St., Las Cruces, NM 88003
Cristina Chiappini
Affiliation:
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, CH-1290 Sauverny, Switzerland
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Abstract

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Sulfur abundances are derived for a sample of ten B MS star members of the Orion association. The analysis is based on LTE model atmospheres and non-LTE line formation theory by means of spectrum synthesis analysis of Sii and Siii lines. The abundance distribution obtained for the Orion targets is homogeneous within the errors in the analysis: A(S)=7.15±0.05. This abundance result is in agreement with the solar value and with results for the Orion nebula. The sulfur abundances for Orion combined with previous results for other OB-type stars produce a relatively shallow sulfur abundance gradient with a slope of −0.037±0.012 dex Kpc−1.

Keywords

stars: early-typestars: abundances(Galaxy:) open clusters and associations: individual (Ori OB1)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 358 - 359
Copyright
Copyright © International Astronomical Union 2010

References

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