Energy Conservation in the thin layer approximation: I. The spherical classic case for supernovae remnants

Abstract

The thin layer approximation applied to the expansion of a supernova remnant assumes that all the swept mass resides in a thin shell. The law of motion in the thin layer approximation is therefore found using the conservation of momentum. Here we instead introduce the conservation of energy in the framework of the thin layer approximation. The first case to be analysed is that of an interstellar medium with constant density and the second case is that of 7 profiles of decreasing density with respect to the centre of the explosion. The analytical and numerical results are applied to 4 supernova remnants: Tycho, Cas A, Cygnus loop, and SN 1006. The back reaction due to the radiative losses for the law of motion is evaluated in the case of constant density of the interstellar medium.

15 pages and 6 figures

References in corpus (7)

• The Structure of Cold Dark Matter Halos
• Proper Motions and Brightness Variations of Nonthermal X-ray Filaments in the Cassiopeia A Supernova Remnant
• An X-ray and Radio Study of the Varying Expansion Velocities in Tycho's Supernova Remnant
• Asymmetric Ejecta Distribution in SN 1006
• Supernova Remnant Crossing a Density Jump: A Thin Shell Model
• Classical and relativistic flux of energy conservation in astrophysical jets
• Classical and relativistic conservation of momentum flux in radio-galaxies

Cited by in corpus (4)

• Energy Conservation in the thin layer approximation: III. The spherical relativistic case for supernovae
• Energy Conservation in the thin layer approximation: IV. The light curve for supernovae
• Energy Conservation in the thin layer approximation: II. The asymmetric classic case for supernovae remnants
• Energy Conservation in the thin layer approximation: V. The surface brightness in supernova remnants