Hostname: page-component-745bb68f8f-s22k5 Total loading time: 0 Render date: 2025-01-31T08:01:31.410Z Has data issue: false hasContentIssue false
  • English
  • Français

Simulations of the evolution of the X-Ray properties of a young stellar population

Published online by Cambridge University Press:  24 November 2004

M. Eracleous ,
M. S. Sipior ,
S. Sigurdsson  and
H. Flohic
M. Eracleous
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
M. S. Sipior
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA Present address: Astronomical Institute “Anton Pannekoek” and Section Computational Science, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, Netherlands.
S. Sigurdsson
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
H. Flohic
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present an X-ray binary population synthesis model, and use it to simulate the evolution of X-ray binaries formed in a burst of star formation of duration 20 Myr and star-formation rate 10 M$_{\odot}$ yr−1. We find that the X-ray luminous phase persists long after the star-formation episode has ended. The 2-10 keV X-ray luminosity can reach values of 1040−1041 erg s−1, comparable to those of some Seyfert galaxies. These models are directly applicable to starburst galaxies as well as LINERs powered by vigorous star formation.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
POSTERS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 165 - 166
Copyright
© 2004 International Astronomical Union