Shock Wave Structure in the Cygnus Loop
The interaction of an SNR blastwave with clouds of various sizes determines the appearance of the SNR in all wavelength bands, and it may determine the overall evolution of the remnant. The Cygnus Loop provides excellent examples of the interaction with both large and small clouds at various stages, and its brightness, large size and low reddening make it a natural target for study. We consider X-ray, optical and UV observations of features at the eastern edge of the Cygnus Loop to look for evidence of cloud evaporation, turbulent stripping from a cloud and pressure enhancement associated with the blastwave-cloud interaction. We consider the effects of the sputtering of dust grains on the temperature derived from ROSAT spectra and we briefly consider the dumpiness of Ha emission to be expected from compression of a turbulent magnetic field.
KeywordsBlast Wave Surface Brightness Density Jump Shock Wave Structure Small Cloud
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