Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ncimb..72..149k&link_type=abstract
Nuovo Cimento B, Serie 11, vol. 72 B, Dec. 11, 1982, p. 149-156.
Astronomy and Astrophysics
Astrophysics
3
Interstellar Gas, Shock Wave Propagation, Spherical Waves, Astronomical Models, Astrophysics, Density Distribution, Numerical Integration, Particle Motion, Propagation Velocity
Scientific paper
The propagation of spherical shock waves through a self-gravitating gas having an initial density distribution rho0 = (beta)(r exp -w) is investigated using the Chisnell-Chester-Whitham method. Analytical expressions for shock velocity and shock strength are derived along with expressions for the pressure, density, and particle velocity immediately behind the shock. It is shown that as the shock advances the shock velocity continuously decreases, whereas for weak shock it initially decreases, attains a minimum value for a certain propagation distance, and then starts increasing. The shock will be relatively strengthened or weakened as w is greater or less than A+2. The case w = A+2 corresponds to the shock moving with constant strength. This case is astrophysically important because of the fact that radial velocity observations of most novae in the course of their outbursts indicate velocities of expansion which remain more or less constant for several days.
Kumar Sanjeev
Saxena D. K.
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