Time-Dependent Models for a decade of SN 1993J

Abstract

A classical and a relativistic law of motion for a supernova remnant (SNR) are deduced assuming an inverse power law behavior for the density of the interstellar medium and applying the thin layer approximation. A third equation of motion is found in the framework of relativistic hydrodynamics with pressure, applying momentum conservation. These new formulas are calibrated against a decade of observations of \snr. The existing knowledge of the diffusive processes of ultrarelativistic electrons is reviewed in order to explain the behavior of the `U' shaped profile of intensity versus distance from the center of SN 1993J.

20 pages 19 figures, Accepted for pubblication in Astrophysics and Space Science 2011

References in corpus (1)

• An introduction to relativistic hydrodynamics

Cited by in corpus (11)

• On the spherical-axial transition in supernova remnants
• Evolution of superbubbles in a self-gravitating disk
• A classical and a relativistic law of motion for spherical supernovae
• Padé approximant for the equation of motion of a supernova remnant
• Energy Conservation in the thin layer approximation: III. The spherical relativistic case for supernovae
• The physics of the optical light curve in supernovae
• The physics of asymmetric supernovae and supernovae remnants
• Analytical and Monte Carlo results for the surface-brightness diameter relationship in supernova remnants
• Energy Conservation in the thin layer approximation: IV. The light curve for supernovae
• Classical and relativistic laws of motion for spherical supernovas
• Classical and relativistic models for time duration of gamma-ray bursts