Physics
Scientific paper
Aug 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmns.proge..10m&link_type=abstract
Presented at the KITP Miniprogram: R-Modes in Neutron Stars, Aug 2, 2000, Kavli Institute for Theoretical Physics, University of
Physics
Scientific paper
Scattering off quantized vortices causes an unique form of dissipation to occurin superfluids known as mutual friction. In superfluid neutron stars mutualfriction is due to the scattering of normal-fluid electrons off quantizedmagnetic-flux carrying neutron vortices. The purpose of this talk is to explainexactly what mutual friction is, how one calculates the mutual friction dampingrate, and what effects this has on the onset of the gravitational-radiationinstability of the r-modes in superfluid neutron stars. The talk begins byreviewing the salient features of superfluidity in neutron stars. It thendiscusses mutual friction in detail. It ends with the results for the stabilityanalysis of ther-modes. The last overhead is an estimate of the effects of mutual friction ina viscousboundary layer.The results shown here are published in L. Lindblom and G. Mendell, Phys. Rev.D61, 104003 (2000), and can be found online at gr-qc/9909084. The abstract fromthat paper follows.The analogs of r-modes in superfluid neutron stars are studied here. Thesemodes, which are governed primarily by the Coriolis force, are identical totheir ordinary-fluid counterparts at the lowest order in the smallangular-velocity expansion used here. The equations that determine the nextorder terms are derived and solved numerically for fairly realistic superfluidneutron-star models. The damping of these modes by superfluid ``mutualfriction'' (which vanishes at the lowest order in this expansion) is found tohave a characteristic time-scale of about 10^4 s for the m=2 r-mode in a``typical'' superfluid neutron-star model. This time-scale is far too long toallow mutual friction to suppress the recently discovered gravitationalradiation driven instability in the r-modes. However, the strength of the mutualfriction damping depends very sensitively on the details of the neutron-starcore superfluid. A small fraction of the presently acceptable range ofsuperfluid models have characteristic mutual friction damping times that areshort enough (i.e. shorter than about 5 s) to suppress the gravitationalradiation driven instability completely. Links to this, and related papers,follow.
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