Numerical Code for Fitting Radial Emission Profile of a Shell Supernova Remnant
High Energy Astrophysical Phenomena
2012-01-05 v1
Abstract
Expressions for surface brightness distribution and for flux density have been theoretically derived in the case of two simple models of a shell supernova remnant. The models are: a homogenous optically thin emitting shell with constant emissivity and a synchrotron shell source with radial magnetic field. Interactive Data Language (IDL) codes for fitting theoretically derived emission profiles assuming these two models to mean profiles of shell supernova remnants obtained from radio observations have been written.
Keywords
Cite
@article{arxiv.1201.0855,
title = {Numerical Code for Fitting Radial Emission Profile of a Shell Supernova Remnant},
author = {Bojan Arbutina and Slobodan Opsenica},
journal= {arXiv preprint arXiv:1201.0855},
year = {2012}
}
Comments
5 pages, 3 figures, XVI National Conference of Astronomers of Serbia, Belgrade, October 10-12, 2011