Analytical methods for the hydrodynamical evolution of supernova remnants.
Abstract
An analytical method for computing the hydrodynamical structure and evolution of supernova remnants (SNRs) is outlined in which the pressure is taken to be a linear function of the mass M(r). Only the onedimensional problem is considered, assuming adiabaticity and plane, cylindrical, or spherical symmetry; most of the calculations are performed in Lagrange coordinates, and the original system of partial differential equations is reduced to a single differential equation involving only time coordinates. The method is applied to the case of Sedov flow and is found to give accurate results. Several less idealized cases are also examined, including the problem of SNR expansion into a hot interstellar medium and early phases of the expansion where the sweptup mass of the interstellar medium is not large compared with the mass of ejecta. The accuracy of the results obtained for these cases is shown to be sufficient for astrophysical applications.
 Publication:

The Astrophysical Journal
 Pub Date:
 October 1978
 DOI:
 10.1086/156506
 Bibcode:
 1978ApJ...225..442G
 Keywords:

 Hydrodynamics;
 Interstellar Matter;
 Shock Wave Propagation;
 Supernova Remnants;
 Density Distribution;
 Gas Expansion;
 Pressure Distribution;
 Astrophysics;
 Evolution:Supernova Remnants;
 Expansion:Supernova Remnants;
 Hydrodynamics:Supernova Remnants