Session 117 - Galactic ISM.
Oral session, Thursday, January 16
Harbour B,

## [117.07] Simulations of Supernova Remnants in the Halo of the Milky Way

R. L. Shelton (NASA/GSFC), D. P. Cox (U. Wisconsin -- Madison)

Hydrodynamic simulations of Supernova Remnants evolving in the halo of our Galaxy will be presented. The results are intriguing.

\beginitemize \item At late times, the remnants collapse faster than the high-stage ions can recombine, thus large numbers of cool C^+3 ions remnain. \item Combining the supernova remnant evolution results with the supernova explosion rates from Ferrière (1995), we find that the high-stage ions in the ensemble of supernova remnants above |z| \simeq 300pc cover \sim 40 % of the northern and southern skies. \item The ensemble provides a large fraction of the observed O^+5. \item 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 \sim 5% of the northern and southern skies. The signal can be very bright, however. \enditemize

Additional results will be presented.

The author(s) of this abstract have provided an email address for comments about the abstract: shelton@olegacy.gsfc.nasa.gov