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Astron. Astrophys. 357, 1157-1169 (2000)

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4. Conclusions

We have derived practical expressions for the bulk viscosity of matter in the cores of neutron stars under conditions in which the bulk viscosity is determined by the direct Urca processes. We have paid special attention to the case in which dense matter consists of neutrons, protons, electrons and muons (Sects. 2.1-2.4). In addition, we have studied the reduction of the bulk viscosity by superfluidity of neutrons and protons (Sect. 3). We have analyzed the cases of singlet-state superfluidity of protons, and triplet-state superfluidity of neutrons (without and with the nodes of superfluid gaps on the nucleon Fermi surface). These cases are most interesting for applications (Sect. 1). We have obtained the practical expressions for the bulk viscosity of superfluid [FORMULA] matter. The results can be used for studying the damping of neutron star pulsations (Sect. 1) and in the studies of the gravitational radiation driven instabilities in rotating neutron stars. We will analyze the bulk viscosity induced by the weaker modified Urca processes (2) in a separate paper.

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© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000
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