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X-Ray Emission from Young Supernovae

Published online by Cambridge University Press:  26 May 2016

Stefan Immler
Stefan Immler*
Affiliation:
Astronomy Department, University of Massachusetts, LGRT-B 528, 710 North Pleasant Street, Amherst, MA 01003, USA
*
1current address: Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802; email: [email protected]

Abstract

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Observations of young SNe in the (∼ 0.1−100 keV) X-ray band allow to establish physical key parameters, such as the circumstellar matter (CSM) density, the mass-loss rate of the progenitor and the temperature of the outgoing and reverse shock as a function of time. Over the last ∼ 25 years, a small number of young SNe has been detected with orbiting X-ray observatories shortly after the outburst (days to months). Some highlights of recent observations with Chandra and XMM-Newton are presented and implications as to our understanding of the physical processes giving rise to the X-ray emission are briefly discussed.

Type
Part 4 Supernovae and Supernova Remnants
Information
Symposium - International Astronomical Union , Volume 214: High Energy Processes and Phenomena in Astrophysics , 2003 , pp. 113 - 116
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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