On the secular instability from thermal conductivity in rotating stars

Details On the secular instability from thermal conductivity in rotating stars On the secular instability from thermal conductivity in rotating stars

Nov 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..974l&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, no. 3, Nov. 1, 1979, p. 974-980. NSF-supported research.

Other

6

Conductive Heat Transfer, Secular Variations, Stellar Models, Stellar Rotation, Thermal Conductivity, Isothermal Flow, Newtonian Fluids, Perturbation Theory, Thermodynamic Properties, Viscous Flow

Scientific paper

A criterion to test the secular stability of rigidly rotating, isothermal Newtonian stellar models is formulated, which includes the dissipative effects of viscosity and thermal conductivity. This criterion reveals a previously unnoticed fact: thermal conductivity can cause secular instability in rotating stellar models. Any stellar model (except for models having degenerate thermodynamic properties such as an incompressible fluid) which is unstable if viscosity is present would also be unstable if the heat conduction coefficient were nonzero. Furthermore, it is shown that the time scale associated with the heat conduction instability can be shorter than the viscous instability time scale.

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