Computer Science
Scientific paper
Sep 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt.........1v&link_type=abstract
Ph.D. Thesis Johns Hopkins Univ., Baltimore, MD.
Computer Science
Light Emission, Luminosity, Shock Waves, Supernova Remnants, Ultraviolet Emission, Ultraviolet Spectrometers, Imaging Techniques, Interstellar Matter, Velocity Distribution, Voyager 1 Spacecraft, Voyager 2 Spacecraft
Scientific paper
Multiwavelength observations are an important tool in the study of supernova remnants (SNR's) on large and small scales. In this thesis, we perform a detailed analysis of two SNR's, the Cygnus Loop and N49. We have used the Voyager 1 and 2 Ultraviolet Spectrometers to study the far-ultraviolet (FUV) emission from the Cygnus Loop. We find widespread emission from O VI lambda lambda 1032, 1038, and C III lambda 977 and we estimate total luminosities in these lines. We create the first FUV images of this remnant. Nonradiative and incomplete shocks contribute substantially to the FUV emission. We find that shocks with velocities greater than or equal to 160 km/s must be widespread even in the optically bright regions. We present a detailed imaging and spectroscopic study of N49 and find that most of the ultraviolet and optical emission emanates from shocks with velocities less than or equal to 140 km/s. However, O VI emission arises behind shocks with velocities approximately 200 km/s. A power-law shock velocity distribution corresponding to 40 km/s less than or equal to Vs less than or equal to 270 km/s provides a good match to the data. We derive improved abundances for N49 and conclude by discussing implications for the interstellar medium surrounding the SNR. We develop a model invoking a Sedov solution in which the main blast wave also encounters large interstellar clouds. For this model, we demonstrate that the energies of N49's evolution as a whole and blast wave/cloud interactions on a smaller scale are self-consistent. Finally, we have constructed models that for the first time predict the dynamic evolution and emission properties of grains behind nonradiative shock waves. We predict observable IR grain and x ray plasma emissions, and we study the effects of varying the preshock density and shock velocity. Our predictions compare favorably to observations of the Cygnus Loop primary shock at IR and x ray energies.
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