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We present IDL (Interactive Data Language) codes for fitting a theoretical   emission profile of a shell supernova remnant (SNR) to the mean profile of an   SNR obtained from radio observations. Two considered theoretical models are:   1) a shell with constant emissivity and 2) a synchrotron shell with radially   aligned magnetic field. The codes were applied to several observed supernova   remnants. Good results are obtained in five considered cases, which justify   the use of our code for remnants that are bright (so that observational   errors are not large) and spherically symmetric enough

Numerical code for fitting radial emission profile of a shell supernova remnant: Application