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Probing interstellar magnetic fields with Supernova remnants

Published online by Cambridge University Press:  01 November 2008

Roland Kothes  and
Jo-Anne Brown
Roland Kothes
Affiliation:
National Research Council of Canada, Herzberg Institute of Astrophysics, Dominion Radio Astrophysical Observatory, P.O. Box 248, Penticton, British Columbia, V2A 6J9, Canada email: [email protected]
Jo-Anne Brown
Affiliation:
Department of Physics and Astronomy, University of Calgary, 2500 University Drive N.W., Calgary, AB, Canada email: [email protected]
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Abstract

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As Supernova remnants expand, their shock waves are freezing in and compressing the magnetic field lines they encounter; consequently we can use Supernova remnants as magnifying glasses for their ambient magnetic fields. We will describe a simple model to determine emission, polarization, and rotation measure characteristics of adiabatically expanding Supernova remnants and how we can exploit this model to gain information about the large scale magnetic field in our Galaxy. We will give two examples: The SNR DA530, which is located high above the Galactic plane, reveals information about the magnetic field in the halo of our Galaxy. The SNR G182.4+4.3 is located close to the anti-centre of our Galaxy and reveals the most probable direction where the large-scale magnetic field is perpendicular to the line of sight. This may help to decide on the large-scale magnetic field configuration of our Galaxy. But more observations of SNRs are needed.

Keywords

Magnetic fields – polarization – ISM: individual (DA 530, G182.4+4.3) – ISM: magnetic fields – Supernova remnants
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 75 - 80
Copyright
Copyright © International Astronomical Union 2009

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