Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..248h&link_type=abstract
Astrophysical Journal, Part 1, vol. 266, Mar. 1, 1983, p. 248-254.
Astronomy and Astrophysics
Astrophysics
Dynamic Stability, Neutron Stars, Newtonian Fluids, Orbit Perturbation, Stellar Models, Stellar Rotation, Canonical Forms, Energy Dissipation, Equations Of Motion, Stellar Gravitation, Stellar Radiation, Thermal Conductivity, Viscosity
Scientific paper
A criterion to test the secular stability of rotating Newtonian stellar models against axisymmetric perturbations is developed. The equilibrium stellar model is assumed to be composed of a dissipative fluid whose shear viscosity coefficient is negligibly smaller than its thermal conductivity and/or bulk viscosity. Such a situation will arise in a neutron star if the dominant form of dissipation is neutrino transport. The new criterion is useful in two situations not covered by previous criteria. First, the effects of thermal conductivity and/or bulk viscosity on secular stability may be studied in differentially rotating stars. Second, gravitational radiation reaction, bulk viscosity, and thermal conductivity may be treated together; separate criteria for the different forms of dissipation are unnecessary. In both cases, it is necessary to restrict attention to axisymmetric perturbations to obtain a usable stability criterion.
No associations
LandOfFree
On axisymmetric perturbations of some rotating stars 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 On axisymmetric perturbations of some rotating stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On axisymmetric perturbations of some rotating stars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1465815