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In this work, we have constructed a relation between the surface brightness $(\Sigma)$ and diameter (D) of Galactic C- and S-type supernova remnants (SNRs). In order to calibrate the $\Sigma$-D dependence, we have carefully examined some intrinsic (e.g. explosion energy) and extrinsic (e.g. density of the ambient medium) properties of the remnants and, taking into account also the distance values given in the literature, we have adopted distances for some of the SNRs which have relatively more reliable distance values. These calibrator SNRs are all C- and S-type SNRs, i.e. F-type SNRs (and S-type SNR Cas A which has an exceptionally high surface brightness) are excluded. The $\Sigma$-D relation has 2 slopes with a turning point at $D=36.5\,\hbox{pc}$: $\Sigma(\hbox{at } 1\,\hbox{GHz})=8.4_{-6.3}^{+19.5} \times 10^{-12}\ D^{-5.99_{-0.33}^{+0.38}} \,\hbox{W}\,\hbox{m}^{-2}\,\hbox{Hz}^{-1}\,\hbox{ster}^{-1}$ (for $\Sigma \leq 3.7\, \times 10^{-21}\,\hbox{W}\,\hbox{m}^{-2}\,\hbox{Hz}^{-1}\,\hbox{ster}^{-1}$ and $D\geq 36.5\,\hbox{pc}$) and $\Sigma(\hbox{at } 1\,\hbox{GHz})=2.7_{-1.4}^{+2.1}\times 10^{-17} D^{-2.47_{-0.16}^{+0.20}}\,\hbox{W}\,\hbox{m}^{-2} \hbox{Hz}^{-1}\,\hbox{ster}^{-1}$ (for $\Sigma \gt 3.7 \times 10^{-21}\,\hbox{W}\,\hbox{m}^{-2}\,\hbox{Hz}^{-1}\,\hbox{ster}^{-1}$ and $D\lt 36.5\,\hbox{pc}$). We discussed the theoretical basis for the $\Sigma\ndash D$ dependence and particularly the reasons for the change in slope of the relation were stated. Added to this, we have shown the dependence between the radio luminosity and the diameter which seems to have a slope close to zero up to about $D=36.5\,\hbox{pc}$. We have also adopted distance and diameter values for all of the observed Galactic SNRs by examining all the available distance values presented in the literature together with the distances found from our $\Sigma \ndash D$ relation.

Keywords: Supernova remnant; distance; neutron star

Document Type: Research Article


Affiliations: 1: Department of Physics, University of Akdeniz, Antalya, Turkey 2: Bogazici Uni.--TUBITAK, Feza Cicersey Institute, 81220 Cengelkoy, Istanbul, Turkey 3: Physics Institute, Academy of Science, Baku 370143, Azerbaijan Republic

Publication date: 2003-06-01

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