Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....96..283p&link_type=abstract
Astronomy and Astrophysics, vol. 96, no. 1-2, Mar. 1981, p. 283-292.
Astronomy and Astrophysics
Astrophysics
9
Astrophysics, Hydrodynamics, Ionization, Stellar Structure, Supernova Remnants, Gas Pressure, Shock Wave Propagation, Stellar Evolution, Time Dependence
Scientific paper
A pseudo-consistent method devised to compute the structure of the remnant decoupling the hydrodynamical and time-dependent ionization computations is described. The dynamical evolution of the dense shell is found to be fairly complex, matter with different velocity being accreted at both edges of the shell. Toward the end of the shock-collapsing phase more than 1000 solar masses of swept-up material are compressed in less than 4% of the remnant volume, carrying approximately 10% of the initial blast energy as bulk kinetic energy. Time-dependent effects are found to be extremely important in determining the ionization structure of the shell, the amount of neutral matter predicted by steady-state collisional ionization equilibrium being much larger than that derived from the present computations. The inability of steady-flow computations of post-shock structure to reproduce quantitatively the complexity of SNR structures is also discussed.
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