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Synthetic UV spectra of starburst regions with massive close binaries

Published online by Cambridge University Press:  26 May 2016

Houria Belkus ,
Joris Van Bever ,
Dany Vanbeveren  and
Walter van Rensbergen
Houria Belkus
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, België
Joris Van Bever
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, België
Dany Vanbeveren
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, België
Walter van Rensbergen
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, België

Abstract

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We present the evolution of synthetic ultraviolet spectra of starburst regions having a significant fraction of binaries. The population synthesis program uses an extended library of stellar evolutionary tracks of single stars and binaries computed with the most recent stellar wind mass loss rates during RSG, LBV and WR stages. In the case of binaries we account in detail for the effects of Roche lobe overflow, mass transfer and mass accretion, common envelope evolution, the spiral-in process, asymmetric kicks to neutron stars as a result of their supernova explosion, etc. The most important synthesized line profiles are those of Si iv λ1400 and C iv λ1550, two P-Cygni lines prominent in O-type stars. The main effect of the close binaries is to extend the UV bright lifetime of the starburst due to the appearance of accretion stars. But more importantly, our computations show that a spectrum of a single star model of about 6 Myr old is effectively undistinguishable from that of a binary rich model of about 10 Myr old. This indicates a possible age degeneracy, reminiscent of the influence of binaries on the commonly used optical age indicator WHβ.

Type
Part 3. Location and Distribution of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 539 - 540
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Belkus, H., Van Bever, J., Vanbeveren, D., van Rensbergen, W. 2002, A&A submitted.Google Scholar
de Mello, D.F., Leitherer, C., Heckman, T.M. 2000, ApJ 530, 251.Google Scholar
Leitherer, C., Robert, C., Heckman, T.M. 1995, ApJS 99, 173.CrossRefGoogle Scholar
Lejeune, T., Cuisinier, F., Buser, R. 1997, A&A 125, 229.Google Scholar
Robert, C., Leitherer, C., Heckman, T.M. 1993, ApJ 418, 749.Google Scholar
Schmutz, W., Leitherer, C., Gruenwald, R. 1992, PASP 104, 1164.Google Scholar
Vanbeveren, D., De Donder, E., Van Bever, J., van Rensbergen, W. 1998, New Astron. 3, 443.Google Scholar
Van Bever, J., Belkus, H., Vanbeveren, D., van Rensbergen, W. 1999, New Astron. 4, 173.Google Scholar