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Connections between jet formation and multiwavelength spectral evolution in black hole transients

Published online by Cambridge University Press:  24 February 2011

Emrah Kalemci ,
Yoon-Young Chun ,
Tolga Dinçer ,
Michelle Buxton ,
John A. Tomsick ,
Stephane Corbel  and
Philip Kaaret
Emrah Kalemci
Affiliation:
Sabanci University, Tuzla İstanbul, Turkey email: [email protected]
Yoon-Young Chun
Affiliation:
Sabanci University, Tuzla İstanbul, Turkey email: [email protected]
Tolga Dinçer
Affiliation:
Sabanci University, Tuzla İstanbul, Turkey email: [email protected]
Michelle Buxton
Affiliation:
Department of Astronomy, Yale University, P.O. Box 208101 New Haven, CT 06520-8101, USA
John A. Tomsick
Affiliation:
Space Sciences Laboratory, University of California, Berkeley 7 Gauss Way, Berkeley, CA 94720-7450, USA
Stephane Corbel
Affiliation:
Laboratoire Astrophysique des Interactions Multi-echelles (UMR 7158) CEA/DSM-CNRS-Universite Paris Diderot CEA Saclay, F-91191 Gif sur Yvette, France
Philip Kaaret
Affiliation:
Department of Physics and Astronomy, University of Iowa Van Allen Hall, Iowa City, IA 52242, USA
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Abstract

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Multiwavelength observations are the key to understand conditions of jet formation in Galactic black hole transient (GBHT) systems. By studying radio and optical-infrared evolution of such systems during outburst decays, the compact jet formation can be traced. Comparing this with X-ray spectral and timing evolution we can obtain physical and geometrical conditions for jet formation, and study the contribution of jets to X-ray emission.

In this work, first X-ray evolution - jet relation for XTE J1752-223 will be discussed. This source had very good coverage in X-rays, optical, infrared and radio. A long exposure with INTEGRAL also allowed us to study gamma-ray behavior after the jet turns on. We will also show results from the analysis of data from GX 339-4 in the hard state with SUZAKU at low flux levels. The fits to iron line fluorescence emission show that the inner disk radius increases by a factor of >27 with respect to radii in bright states. This result, along with other disk radius measurements in the hard state will be discussed within the context of conditions for launching and sustaining jets.

Keywords

accretionblack hole physicsline: profiles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 299 - 302
Copyright
Copyright © International Astronomical Union 2011

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