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X-ray Emission as an Indicator of Cosmic ray Acceleration in Supernova Remnants

Published online by Cambridge University Press:  25 May 2016

R. Petre ,
G. E. Allen ,
U. Hwang ,
J. W. Keohane  and
E. V. Gotthelf
R. Petre
Affiliation:
Laboratory for High Energy Astrophysics, Goddard Space Flight Center, Greenbelt, MD 20771, U.S.A.
G. E. Allen
Affiliation:
NASA / Chandra X-Ray Center, Massachusetts Institute of Technology, Cambridge MA, 02139, U.S.A.
U. Hwang
Affiliation:
Goddard Space Flight Center and University of Maryland, Greenbelt, MD 20771, U.S.A.
J. W. Keohane
Affiliation:
NASA / North Carolina School of Science and Mathematics, Durham, NC 27705, U.S.A.
E. V. Gotthelf
Affiliation:
Astronomy Department, Columbia University, New York, NY 10027, U.S.A.

Abstract

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X-ray observations over the past several years have led to the discovery of nonthermal X-ray emission arising in the shells of many young supernova remnants, including SN 1006, Cas A, and Tycho. This emission is thought to be synchrotron emission from electrons that have been shock accelerated to hundreds of TeV, and thus represents strong evidence that cosmic rays are accelerated in SNR shocks. The X-ray observations are corroborated by detection of TeV gamma rays from two of these remnants. A systematic investigation of young, shell-like remnants suggests that the nonthermal X-ray emission from shock-accelerated electrons is a common, if not ubiquitous, feature. We review the status of the X-ray observations and describe how they can be used to provide insight into the shock acceleration process.

Type
Part I: Talks
Information
Symposium - International Astronomical Union , Volume 195: Highly Energetic Physical Processes and Mechanisms , 2000 , pp. 69 - 76
Copyright
Copyright © Astronomical Society of the Pacific 2000 

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