Statistics – Computation
Scientific paper
Aug 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..648d&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 2, p. 648-663.
Statistics
Computation
10
Interstellar Matter, Radio Emission, Stellar Evolution, Supernova Remnants, Taylor Instability, Astronomical Models, Computational Astrophysics, Hydrodynamic Equations
Scientific paper
During the evolution of a supernova remnant (SNR), some of the explosion energy is converted to relativistic electron energy at the shock front, and turbulent dynamo processes associated with the growth of Rayleigh-Taylor (R-T) fingers convert explosion kinetic energy into magnetic field energy. Phenomenological descriptions of these processes have been incorporated into a one-dimensional, spherical hydrodynamics program. Input parameters used in the calculations included the explosion energy, the mean circumstellar medium (CSM) density, and various characteristics of the clump CSM. In this paper, the evolution of global properties such as total magnetic energy and luminosity are related to the input parameters through the use of power-law fits and heuristic scaling functions. The results show that, once an SNR reaches the Sedov phase of evolution, it evolves along a track parallel to the observed surface brightness (Sigma)-diameter (D) relation for Galactic and Magellanic Cloud SNRs. We conclude that the observed range in surface brightness for a given diameter (a factor of about 30) is probably the result of variations in explosion energy (up to a factor of 8) and/or in the contrast between the mean CSM density and the peak density of individual clumps (up to a factor of 20).
Dickel John R.
Eilek Jean A.
Jones Eric M.
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