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Simulations of Halo Supernova Remnants

Published online by Cambridge University Press:  12 April 2016

R.L. Shelton
R.L. Shelton*
Affiliation:
Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD 20706, USA.

Abstract

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High latitude observations find C3+, N4+, and O5+, while shadowing by intervening hydrogen clouds indicates the presence of soft X-ray emitting gas in the halo of our galaxy. This paper reports on detailed hydrocode simulations of one of the possible source types: isolated supernova remnants evolving in the tenuous ambient medium of the halo. Their O5+ column densities are similar to those observed from the halo. The N4+, C3+, and X-ray properties are also simulated and discussed. The calculations may also be of interest for the Local Bubble, external galaxies, and non-thermal pressure estimations.

Type
Part VII Gas in Superbubbles and in the Galactic Halo
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 443 - 446
Copyright
Copyright © Springer-Verlag 1998

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