UV Spectra of Evolved Magellanic Cloud Supernova Remnants

Details UV Spectra of Evolved Magellanic Cloud Supernova Remnants UV Spectra of Evolved Magellanic Cloud Supernova Remnants

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1778b&link_type=abstract

IUE Proposal ID #NEGWB

Mathematics

Scientific paper

We wish to obtain SWP spectra of three supernova remnants (SNRs) in the Large Magellanic Cloud and one in the Small Magellanic Cloud for purposes of studying SNR evolution and grain destruction processes in these galaxies. The UV spectra will allow us to determine the shock velocity and carbon and silicon abundances for each of the remnants. In conjunction with optical data, the shock velocity will allow us to estimate the pressure within each remnant. By determining the pressure as a function of diameter we will investigate whether the remnants are in the free expansion phase (as suggested by Mathewson et al., 1983) or the adiabatic phase (as suggested by previous investigators). The carbon and silicon abundances will be compared to results from H II regions to determine if grain destruction has taken place in the SNR shocks.

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