Superfluid effects on thermal evolution and rotational dynamics of neutron stars

Details Superfluid effects on thermal evolution and rotational dynamics of neutron stars Superfluid effects on thermal evolution and rotational dynamics of neutron stars

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001phdt.........2l&link_type=abstract

Thesis (PhD). MONTANA STATE UNIVERSITY, Source DAI-B 62/02, p. 898, Aug 2001, 81 pages.

Physics

2

Scientific paper

This thesis examines the observational consequences of superfluidity on thermal evolution and rotational dynamics of neutron stars. Temperature measurements of older neutron stars (tage >~ 106 yrs) indicate that these objects are heated. A promising candidate heat source is friction due to differential rotation between the neutron star crust and the superfluid it is thought to contain. We study the effects of superfluid friction on the long-term thermal and rotational evolution of a neutron star and obtain constraints on the strength of the frictional coupling between the stellar crust and the interior superfluid. The second part of this thesis provides simulations of glitches (sudden jumps in spin rate) in isolated pulsars. With the aim of distinguishing among different theoretical explanations for the glitch phenomenon, we study the response of a neutron star to two types of perturbations to the vortex array that threads the superfluid interior. Both mechanisms produce acceptable fits to glitch observations in the four pulsars we study. The two models make different predictions for the generation of internal heat and subsequent enhancement of surface emission. Future glitch observations coordinated with surface emission measurements will play a key role in distinguishing between the two glitch models we investigate.

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