Statistics – Computation
Scientific paper
Jan 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...190..320b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 190, no. 1-2, Jan. 1988, p. 320-332.
Statistics
Computation
10
Astronomical Models, Conductive Heat Transfer, Supernova Remnants, Computational Astrophysics, Heat Flux, Hydrodynamic Equations, Plasma Turbulence, Shock Waves, Stellar Winds
Scientific paper
The problem of heat conduction in young SNRs is studied by modeling the ejected material as a uniformly expanding gas in which the inner 4/7 of the stellar mass has constant density and the outer 3/7 has a profile with rho proportional to r exp -7. The interaction of this profile with the circumstellar medium is computed, including electron thermal conduction, in the context of two-fluid numerical hydrodynamics. Two limiting cases (total or no energy equipartition between ions and electrons on the shock) are considered. In the first case thermal conduction appears to drive instabilities in the fluid motion. This behavior was confirmed also in different contexts such as the model of Hamilton and Sarazin (1984) and the two-colliding-winds problem. The effects of the instabilities are considered and discussed in the light of the radio and X-ray observations of young SNRs such as Tycho and Cas A.
Bedogni R.
D'Ercole Annibale
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