Bulk viscosity in hyperonic star and r-mode instability

Abstract

We consider a rotating neutron star with the presence of hyperons in its core, using an equation of state in an effective chiral model within the relativistic mean field approximation. We calculate the hyperonic bulk viscosity coefficient due to nonleptonic weak interactions. By estimating the damping timescales of the dissipative processes, we investigate its role in the suppression of gravitationally driven instabilities in the $r$-mode. We observe that $r$-mode instability remains very much significant for hyperon core temperature of around $10^8$K, resulting in a comparatively larger instability window. We find that such instability can reduce the angular velocity of the rapidly rotating star considerably upto $\sim 0.04{\Omega }_K$, with ${\Omega }_K$ as the Keplerian angular velocity.

10 pages including 7 figures

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Cited by in corpus (13)

• Neutron Stars and the Nuclear Equation of State
• Do hyperons exist in the interior of neutron stars ?
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• Transport coefficients in Polyakov quark meson coupling model: a relaxation time approximation
• Hyperon bulk viscosity and $r$-modes of neutron stars
• Non-radial oscillations in anisotropic dark energy stars
• Tidal heating as a direct probe of strangeness inside neutron stars
• Properties of strongly magnetized ultradense matter and their imprints on magnetar pulsations
• Effects of dark boson mediated feeble interaction between dark matter (DM) and quark matter on $f$-mode oscillation of DM admixed quark stars
• Tidal dissipation in binary neutron star inspirals from hyperon bulk viscosity: Phase modeling and parameter estimation bias
• r-mode instability of neutron stars in low-mass X-ray binaries: effects of Fermi surface depletion and superfluidity of dense matter
• Magnetic field generated by r-modes in accreting quark stars