New instability windows for rotating neutron stars
نویسندگان
چکیده
We reanalyze the r-mode instability in rotating superfluid neutron stars. To this aim we develop a model of resonance interaction of normal m = 2 r-mode with superfluid modes. We show that this interaction dramatically modifies the instability window, that is the region of stellar spin frequencies and temperatures in which a neutron star becomes unstable with respect to radiation of gravitational waves. This modification allows us to formulate an evolution scenario for neutron stars in LMXBs that can explain all rapidly rotating neutron stars observed in LMXBs, as well as the existence of millisecond pulsars (see arXiv:1305.3825 and the presentation ‘Observationally consistent evolution scenario for neutron stars in LMXBs’ by Gusakov, Chugunov, and Kantor for more details).
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