Mutual friction in a cold color flavor locked superfluid and r-mode instabilities in compact stars

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dc.creatorMannarelli, Massimo
dc.creatorManuel, Cristina
dc.creatorSa'd, Basil A.
dc.date2008-07-21
dc.date2008-12-15
dc.date.accessioned2026-07-07T12:27:28Z
dc.date.available2026-07-07T12:27:28Z
dc.descriptionDissipative processes acting in rotating neutron stars are essential in preventing the growth of the r-mode instability. We estimate the damping time of r-modes of an hypothetical compact quark star made up by color flavor locked quark matter at a temperature $T \lesssim 0.01$ MeV. The dissipation that we consider is due to the the mutual friction force between the normal and the superfluid component arising from the elastic scattering of phonons with quantized vortices. This process is the dominant one for temperatures $T \lesssim 0.01$ MeV where the mean free path of phonons due to their self-interactions is larger than the radius of the star and they can be described as an ideal bosonic gas. We find that r-modes oscillations are efficiently damped by this mechanism for pulsars rotating at frequencies of the order of 1 Hz at most. Our analysis rules out the possibility that cold pulsars rotating at higher frequencies are entirely made up by color flavor locked quark matter.
dc.description4 pages; comments and refs. added; it matches with published version
dc.identifierhttps://arxiv.org/abs/0807.3264
dc.identifierhttp://arxiv.org/abs/0807.3264
dc.identifierPhys.Rev.Lett.101:241101,2008
dc.identifierdoi:10.1103/PhysRevLett.101.241101
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/215216
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectAstrophysics
dc.subjectNuclear Theory
dc.titleMutual friction in a cold color flavor locked superfluid and r-mode instabilities in compact stars
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