Physics
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1806f&link_type=abstract
IUE Proposal ID #IMGRF
Physics
Scientific paper
Little is known about the properties of extremely old supernova. remnants (SNRs) due to their weak or undetectable optical and radio emissions. Yet, it is precisely the last stages in a SNR's evolution which would provide the best estimates of a remnant's total amount of swept-up mass, final size, and elemental depletion, and relationship to high-velocity interstellar clouds. We propose the first direct measurements of some of the basic physical properties of extremely old STIRS via UV interstellar absorption lines observable in the spectra of early-type stars located behind suspected old SNRs. We have identified several large-scale, shell-like dust features which can be plausibly associated with extremely evolved remnants. An archival IUE observation supports our identification procedure as well as the feasibility of studying extremely old SNRs using methods similar to those used for much younger remnants. This new approach of identifying and studying the massive shells (> 10^3 M[sun]) absorption line measurements offers a means of probing the properties of these objects just prior to their merger with the ISM. Spectral data collected at high resolution in the long and short wavelength regions of carefully selected target stars behind and outside the candidate remnant shells can provide direct measurements on several properties of these structures: 1) estimate of maximum dimensions of shells, 2) a measurement of the column density via curve-of-growth analysis leading to an estimate of the shell's total mass, 3) the shell's present kinetic energy and thereby an estimate of the original total energy of SNR, and 4) examination of absorption line strengths for evidence of element depletion by grains.
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