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The Determination of the Abundances of the Fe Group Elements in Early B Stars from High Resolution FUV Spectra

Published online by Cambridge University Press:  09 March 2010

Geraldine J. Peters ,
Saul J. Adelman ,
Ivan Hubeny  and
Thierry Lanz
Geraldine J. Peters
Affiliation:
Space Sciences Center & Dept. of Physics & Astronomy, University of Southern California, Los Angles, CA 90089-1341, USA email: gjpeters@mucen.usc.edu
Saul J. Adelman
Affiliation:
The Citadel, Charleston, SC 29409-0270, USA email: adelmans@citadel.edu
Ivan Hubeny
Affiliation:
University of Arizona, Tucson, AZ 85721-0065, USA email: hubeny@aegis.as.arizona.edu
Thierry Lanz
Affiliation:
University of Maryland, College Park, MD 20742-2421, USA, email: lanz@astro.umd.edu
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Abstract

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We present selected results from an investigation that is currently underway to determine the abundances of the Fe group elements in early B stars and assess the extent to which contemporary NLTE and LTE models represent their atmospheres. High resolution UV and optical spectra of B stars that display ultrasharp lines are compared with computations from TLUSTY/SYNSPEC and SYNTHE. Some results from our analysis of the abundance standard ι Her (B3V) are presented here.

Keywords

stars: abundancesstars: atmospheresstars: early-type
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. 213 - 214
Copyright
Copyright © International Astronomical Union 2010

References

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