Bulk viscosity coefficients due to phonons and kaons in superfluid color-flavor locked quark matter

Bierkandt, Robert; Manuel, Cristina

doi:10.1103/physrevd.84.023004

Cited by 13 publications

(10 citation statements)

References 38 publications

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“…However, the dominant contribution to the bulk viscosity may come from processes involving the neutral kaon K 0 [37,40,41]. For temperatures above a few MeV, the bulk viscosity ζ K 0 can become larger than for unpaired quark matter, but at low temperatures ζ K 0 is much less than that of unpaired quark matter (see also [42]). As a consequence, for cold enough objects we may expect that the fundamental mode will be damped only by gravitational radiation, and the determination of the frequency and damping time of the fundamental mode could be a promising way to constrain the properties of CFL strange stars.…”

Section: Discussionmentioning

confidence: 99%

Constraining color flavor locked strange stars in the gravitational wave era

Flores

Lugones

2017

Phys. Rev. C

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We perform a detailed analysis of the fundamental mode of non-radial pulsations of color flavor locked strange stars. Solving the general relativistic equations for non-radial pulsations for an equation of state derived within the MIT bag model, we calculate the frequency and the gravitational damping time of the fundamental mode for all the parametrizations of the equation of state that lead to self-bound matter. Our results show that color flavor locked strange stars can emit gravitational radiation in the optimal range for present gravitational wave detectors and that it is possible to constrain the equation of state's parameters if the fundamental oscillation mode is observed and the stellar mass is determined. We also show that the f -mode frequency can be fitted as a function of the square root of the average stellar density M/R 3 by a single linear relation that fits quite accurately the results for all parametrizations of the equation of state. All results for the damping time can also be fitted as a function of the compactness M/R by a single empirical relation. Therefore, if a given compact object is identified as a color flavor locked strange star these two relations could be used to determine the mass and the radius from the knowledge of the frequency and the damping time of gravitational waves from the f mode.

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Section: Discussionmentioning

confidence: 99%

Constraining color flavor locked strange stars in the gravitational wave era

Flores

Lugones

2017

Phys. Rev. C

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“…This effective theory does not tell us if and at what density CFL is replaced by another phase, but it can be used to compute properties of CFL and CFL- in terms of a small number of unknown couplings in the Lagrangian. This has been done for transport properties such as bulk and shear viscosities [ 2373 , 2390 – 2392 ]. Since its form is determined by the symmetries of CFL, the effective theory must be valid for all densities where CFL, or any other phase with the same symmetry breaking pattern, exists (at energies far below the critical temperature of CFL).…”

Section: Nuclear Physics and Dense Qcd In Colliders And Compact Starsmentioning

confidence: 99%

“…In quark matter, only the CFL phase (and its variants) is superfluid, because of the spontaneous breaking of baryon number conservation, see ( 7.4 ). Superfluidity of the CFL phase manifests itself-for instance in the presence of three different bulk viscosity parameters [ 2392 ].…”

Section: Nuclear Physics and Dense Qcd In Colliders And Compact Starsmentioning

confidence: 99%

QCD and strongly coupled gauge theories: challenges and perspectives

et al. 2014

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We highlight the progress, current status, and open challenges of QCD-driven physics, in theory and in experiment. We discuss how the strong interaction is intimately connected to a broad sweep of physical problems, in settings ranging from astrophysics and cosmology to strongly coupled, complex systems in particle and condensed-matter physics, as well as to searches for physics beyond the Standard Model. We also discuss how success in describing the strong interaction impacts other fields, and, in turn, how such subjects can impact studies of the strong interaction. In the course of the work we offer a perspective on the many research streams which flow into and out of QCD, as well as a vision for future developments.

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“…In the case of astrophysical phenomena, the bulk viscosities are calculated for periodic perturbations, leading the system away from equilibrium. In [30], it was shown that:…”

Section: Bulk Viscositiesmentioning

confidence: 99%

Transport Properties of Superfluid Phonons in Neutron Stars

Manuel

Tolós

2021

Universe

Self Cite

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We review the effective field theory associated with the superfluid phonons that we use for the study of transport properties in the core of superfluid neutrons stars in their low temperature regime. We then discuss the shear and bulk viscosities together with the thermal conductivity coming from the collisions of superfluid phonons in neutron stars. With regard to shear, bulk, and thermal transport coefficients, the phonon collisional processes are obtained in terms of the equation of state and the superfluid gap. We compare the shear coefficient due to the interaction among superfluid phonons with other dominant processes in neutron stars, such as electron collisions. We also analyze the possible consequences for the r-mode instability in neutron stars. As for the bulk viscosities, we determine that phonon collisions contribute decisively to the bulk viscosities inside neutron stars. For the thermal conductivity resulting from phonon collisions, we find that it is temperature independent well below the transition temperature. We also obtain that the thermal conductivity due to superfluid phonons dominates over the one resulting from electron-muon interactions once phonons are in the hydrodynamic regime. As the phonons couple to the Z electroweak gauge boson, we estimate the associated neutrino emissivity. We also briefly comment on how the superfluid phonon interactions are modified in the presence of a gravitational field or in a moving background.

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Bulk viscosity coefficients due to phonons and kaons in superfluid color-flavor locked quark matter

Cited by 13 publications

References 38 publications

Constraining color flavor locked strange stars in the gravitational wave era

Constraining color flavor locked strange stars in the gravitational wave era

QCD and strongly coupled gauge theories: challenges and perspectives

Transport Properties of Superfluid Phonons in Neutron Stars

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