Thermal-timing instability in neutron stars

Details Thermal-timing instability in neutron stars Thermal-timing instability in neutron stars

Feb 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.277..521g&link_type=abstract

Nature, vol. 277, Feb. 15, 1979, p. 521-523. Research supported by the Research Corp.

Physics

7

Neutron Stars, Pulsars, Stellar Models, Stellar Temperature, Thermal Instability, Angular Velocity, Periodic Variations, Perturbation Theory, Stellar Interiors, Stellar Rotation, Thermal Emission

Scientific paper

If neutron star interiors are superfluid, heat will be frictionally dissipated within them as their rotation slows. It is shown that in certain circumstances this process can become unstable. The frictional generation of heat can undergo a runaway, depositing a significant burst of heat in the star in a short period of time. This runaway is purely thermal in nature. It results from an instability in an energy-generation process. Nevertheless, it has observable effects on the rotation rate of the pulsar. Neutron star interiors rotate more rapidly than their surfaces, and the frictional coupling between the two increases with increasing temperature. A burst of heat, therefore, tends to cause the star to 'seize' up. The inside slows down, and the outside, the pulsar, speeds up. The thermal instability manifests itself through its pulsar timing effects.

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