Computer Science – Sound
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...274..152v&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 274, Nov. 1, 1983, p. 152-167.
Computer Science
Sound
327
Galactic Evolution, Gravitational Effects, Interstellar Gas, Magnetohydrodynamic Stability, Shock Wave Propagation, Stellar Evolution, Astrodynamics, Cosmology, Perturbation Theory, Spherical Waves
Scientific paper
This paper examines the stability of a thin, spherical shock against dynamic and gravitational perturbations when the wavelength of the perturbation is large compared to the thickness of the dense shell. For dynamic perturbations, it is found that a spherical isothermal shock, driven by a hot gas, is overstable against small perturbations. As a result, the fragmentation of the shell proceeds in an oscillatory manner. The smaller wavelength perturbations are most unstable, with the maximum growth rate being comparable to the inverse of the time it takes sound waves to propagate through the shell thickness. The nonradiating case is not subject to this overstability unless d ln P/d ln rho is close to 1. The overstability can appear in cases where there is an ambient magnetic field. The growth of gravitationally driven perturbations is also considered.
No associations
LandOfFree
The dynamic and gravitational instabilities of spherical shocks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The dynamic and gravitational instabilities of spherical shocks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The dynamic and gravitational instabilities of spherical shocks will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1484360