Diffusion as a leading dissipative mechanism in superconducting neutron stars
arXiv:2105.08121 · doi:10.1093/mnrasl/slab078
Abstract
Despite the fact that different particle species can diffuse with respect to each other in neutron star (NS) cores, the effect of particle diffusion on various phenomena associated with NS oscillations is usually ignored. Here we demonstrate that the diffusion can be extremely powerful dissipative mechanism in superconducting NSs. In particular, it can be much more efficient than the shear and bulk viscosities. This result has important implications for the damping times of NS oscillations, development and saturation of dynamical instabilities in NSs, and for the excitation and coupling of oscillation modes during the late inspiral of binary NSs.
arXiv comment6 pages, 3 figures, version accepted for publication in MNRAS Letters
References in corpus (35)
- A new class of unstable modes of rotating relativistic stars
- Neutrino Emission from Neutron Stars
- Axial instability of rotating relativistic stars
- Gravitational waves from instabilities in relativistic stars
- Superfluidity in nuclear systems and neutron stars
- Runaway Heating By R-modes of Neutron Stars in Low Mass X-ray Binaries
- Constraints on Neutron Star Crusts From Oscillations in Giant Flares
- Spin Evolution of Accreting Neutron Stars: Nonlinear Development of the R-mode Instability
- Second-order rotational effects on the r-modes of neutron stars
- Resonant tidal excitation of superfluid neutron stars in coalescing binaries
- The rotational modes of relativistic stars: Analytic results
- The rotational modes of relativistic stars: Numerical results
- Pairing in high-density neutron matter including short- and long-range correlations
- Pairing in high-density neutron matter including short- and long-range correlations
- A hydrodynamical trigger mechanism for pulsar glitches
- R-modes in neutron stars: Theory and observations
- Using gravitational-wave data to constrain dynamical tides in neutron star binaries
- Explaining observations of rapidly rotating neutron stars in LMXBs
- Implications of an r-mode in XTE J1751-305: Mass, radius and spin evolution
- A Non-radial Oscillation Mode in an Accreting Millisecond Pulsar?
- Constraints on the nuclear equation of state and the neutron star structure from crustal torsional oscillations
- Constraining the p-mode--g-mode tidal instability with GW170817
- Composition temperature-dependent g-modes in superfluid neutron stars
- A new method to constrain neutron star structure from quasi-periodic oscillations
- Relativistic dynamics of superfluid-superconducting mixtures in the presence of topological defects and an electromagnetic field with application to neutron stars
- Evolution of the magnetic field in neutron stars
- Growth rate of the tidal p-mode g-mode instability in coalescing binary neutron stars
- Do superfluid instabilities prevent neutron star precession?
- Bulk viscosity in neutron stars with hyperon cores
- Thermal Evolution of a Pulsating Neutron Star
- Dissipative relativistic magnetohydrodynamics of a multicomponent mixture and its application to neutron stars
- Constraining neutron superfluidity with -mode physics
- Transport coefficients of leptons in superconducting neutron star cores
- Temperature-dependent r-modes in superfluid neutron stars stratified by muons
- The Secular Bar-Mode Instability in Rapidly Rotating Stars Revisited
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- Role of particle diffusion in shaping the gravitational wave signal from neutron star inspirals
- Instability windows of relativistic r-modes in stably stratified neutron stars with hyperonic cores
- Dissipative superfluid relativistic magnetohydrodynamics of a multicomponent fluid: the combined effect of particle diffusion and vortices