Computer Science – Numerical Analysis
Scientific paper
Apr 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987phfl...30.1052s&link_type=abstract
Physics of Fluids (ISSN 0031-9171), vol. 30, April 1987, p. 1052-1058.
Computer Science
Numerical Analysis
8
Disk Galaxies, Galactic Evolution, Hydrodynamic Equations, Interstellar Gas, Stress Tensors, Boltzmann Transport Equation, Euler-Lagrange Equation, Integral Equations, Kinetic Theory, Numerical Analysis
Scientific paper
A consistent hydrodynamic model is established to describe the evolution of thin disk galaxies. A previous result showing that the heat flow vanishes in the limit of small epicyclic motion is generalized and simplified, providing a closure relation for the hierarchy of fluid equations. Its systematic use makes it possible to obtain a new invariant of the fluid motion, governing the evolution of the anisotropic pressure (stress) tensor. This might represent a step toward explicit adiabatic laws relating the pressure and the density of the stellar gas. The same closure relation is then used to derive a powerful variational principle, describing linearized perturbations of the system, which takes the pressure anisotropy fully into account. This principle is independent of the usual WKB ('tightly wound') approximation, which is easily recovered in the asymptotic study of spiral waves and spiral modes.
Pellat Rene
Sygnet Jean-Francois
Tagger Michel
No associations
LandOfFree
A hydrodynamic description of disk galaxies 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 A hydrodynamic description of disk galaxies, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A hydrodynamic description of disk galaxies will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1349596