Simulations of Supernova Remnants in the Halo of the Milky Way

Details Simulations of Supernova Remnants in the Halo of the Milky Way Simulations of Supernova Remnants in the Halo of the Milky Way

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...18911707s&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #117.07; Bulletin of the American Astronomical Society, Vol. 28, p.1430

Astronomy and Astrophysics

Astronomy

Scientific paper

Hydrodynamic simulations of Supernova Remnants evolving in the halo of our Galaxy will be presented. The results are intriguing. At late times, the remnants collapse faster than the high-stage ions can recombine, thus large numbers of cool C(+3) ions remain. Combining the supernova remnant evolution results with the supernova explosion rates from Ferriere (1995), we find that the high-stage ions in the ensemble of supernova remnants above |z| =~ 300pc cover ~ 40 % of the northern and southern skies. The ensemble provides a large fraction of the observed O(+5) . While the high-stage ions from an SNR can remain for several million years, the x-ray signal is more fleeting. For example, the Si(+10) from the ensemble covers only ~ 5% of the northern and southern skies. The signal can be very bright, however. Additional results will be presented.

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