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Problems in abundance determination from UV spectra of hot supergiants

Published online by Cambridge University Press:  09 March 2010

M. Sarta Deković ,
D. Kotnik-Karuza ,
T. Jurkić  and
D. Dominis Prester
M. Sarta Deković
Affiliation:
Department of Physics, University of Rijeka, Omladinska 14, 51000 Rijeka, Croatia email: msarta@phy.uniri.hr
D. Kotnik-Karuza
Affiliation:
Department of Physics, University of Rijeka, Omladinska 14, 51000 Rijeka, Croatia email: msarta@phy.uniri.hr
T. Jurkić
Affiliation:
Department of Physics, University of Rijeka, Omladinska 14, 51000 Rijeka, Croatia email: msarta@phy.uniri.hr
D. Dominis Prester
Affiliation:
Department of Physics, University of Rijeka, Omladinska 14, 51000 Rijeka, Croatia email: msarta@phy.uniri.hr
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Abstract

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We present measurements of equivalent widths of the UV, presumably photospheric lines: C III 1247 Å, N III 1748 Å, N III 1752 Å, N IV 1718 Å and He II 1640 Å in high-resolution IUE spectra of 24 galactic OB supergiants. Equivalent widths measured from the observed spectra have been compared with their counterparts in the Tlusty NLTE synthetic spectra. We discuss possibilities of static plan-parallel model to reproduce observed UV spectra of hot massive stars and possible reasons why observations differ from the model so much.

Keywords

stars: abundancesstars: supergiantsultraviolet: stars
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. 211 - 212
Copyright
Copyright © International Astronomical Union 2010

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