Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277..353l&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 2, pp. 353-361.
Astronomy and Astrophysics
Astronomy
4
Hydrodynamics, Line: Profiles, Shock Waves, Supernova Remnants
Scientific paper
Models of multifluid shocks propagating into media of very high pre-shock ionization introduce difficulties in the use of standard hydrodynamic continuity equations to describe the neutral gas and hence reproduce the Hα profiles of these shocks. The problems arise from the lack of thermal contact between the atoms in the neutral component of the shock structure, the model of this component as an ideal gas in thermal equilibrium therefore being inaccurate. We have overcome this problem by explicitly solving a transport equation to obtain the velocity distribution function of the neutral gas. Numerical solutions to this equation, under the physical conditions of a shock transition, are used to follow the evolution of the distribution function. The effect on the neutral distribution function of atomic interactions with the other components of the shock structure can be calculated, and the emitted Hα line profiles can then be obtained. Predicted Hα profiles of shocks with pre-ionization fractions that are so high that the neutral gas makes no significant dynamical contribution to the shock structure are presented for shock velocities between 313 and 2500 km s^-1. These profiles show the two-component structure seen in several observations of filamentary structures in supernova remnants.
Lim Andrew J.
Raga Alejandro C.
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