Postglitch behavior of the plasma inside neutron stars

Easson, I.

doi:10.1086/156842

Cited by 60 publications

(109 citation statements)

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“…The results of the elegant and compact notation of Easson (1979b) are also recovered in the limit K = α = 0; by expanding the real and complex components of his complex function F one obtains F = ∂χ/∂z + iV .…”

Section: Solutionmentioning

confidence: 85%

“…Originally proposed by Baym et al (1969), this assumption has been validated for the slow spin-down of the pulsar frequency produced by magnetic dipole braking (Easson 1979a), as well as for an impulsive change in the pulsar frequency induced by a glitch (Easson 1979b). In the latter case, co-rotation is established by an Ekman-like process, driven by the Coriolis force in the magneto-inertial boundary layers that form immediately after the glitch.…”

Section: Introductionmentioning

confidence: 89%

“…A popular explanation is that they arise when the neutron superfluid, whose angular momentum is frozen by the pinning of superfluid vortices, is suddenly transferred to the crust as a result of avalanche unpinning of the vortex array (Anderson & Itoh 1975;Melatos & Warszawski 2009;Warszawski & Melatos 2008Haskell et al 2012;Warszawski et al 2012). Following the glitch, the crust and core readjust via viscous and magnetic forces (Baym et al 1969), the latter of which is expected to be dominant in all but the oldest pulsars (Easson 1979b).…”

Section: Coupled Response Of a Magnetised Plasma And Its Containermentioning

confidence: 99%

“…The magnetic diffusivity is omitted in Equation (2) as it is expected to be extremely small in neutron stars (Easson 1979b). The stress tensor T is (in index notation)…”

Section: Governing Equationsmentioning

confidence: 99%

“…To solve Equations (11)- (18), we follow previous authors (Greenspan & Howard 1963;Easson 1979b) and consider solutions of the form…”

Section: Solutionmentioning

confidence: 99%

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Short-Period Pulsar Oscillations Following a Glitch

Eysden

2014

ApJ

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Following a glitch, the crust and magnetized plasma in the outer core of a neutron star are believed to rapidly establish a state of co-rotation within a few seconds by process analogous to classical Ekman pumping. However, in ideal magnetohydrodynamics, a final state of co-rotation is inconsistent with conservation of energy of the system. We demonstrate that, after the Ekman-like spin up is completed, magneto-inertial waves continue to propagate throughout the star, exciting torsional oscillations in the crust and plasma. The crust oscillation is irregular and quasi-periodic, with a dominant frequency of the order of seconds. Crust oscillations commence after an Alfvén crossing time, approximately half a minute at the magnetic pole, and are subsequently damped by the electron viscosity over approximately an hour. In rapidly rotating stars, the magneto-inertial spectrum in the core approaches a continuum, and crust oscillations are damped by resonant absorption analogous to quasi-periodic oscillations in magnetars. The oscillations predicted are unlikely to be observed in timing data from existing radio telescopes, but may be visible to next generation telescope arrays.

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Section: Solutionmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 89%

Section: Coupled Response Of a Magnetised Plasma And Its Containermentioning

confidence: 99%

“…The magnetic diffusivity is omitted in Equation (2) as it is expected to be extremely small in neutron stars (Easson 1979b). The stress tensor T is (in index notation)…”

Section: Governing Equationsmentioning

confidence: 99%

“…To solve Equations (11)- (18), we follow previous authors (Greenspan & Howard 1963;Easson 1979b) and consider solutions of the form…”

Section: Solutionmentioning

confidence: 99%

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Short-Period Pulsar Oscillations Following a Glitch

Eysden

2014

ApJ

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Spin density polarization effects in the presence of Coriolis force on ion acoustic waves in quantum plasma

Hussain

Abdikian

Hasnain

2020

Contributions to Plasma Physics

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Ion acoustic solitary waves in a quantum plasma, which is slowly rotating around an axis at an angle θ with the direction of magnetic field, are investigated. Quantum hydrodynamic model is under consideration with the effects of rotations which are included via Coriolis force. Fermions are degenerate and have different spin density states, that is, up and down characterized via parameter α. Linear analysis is performed by applying Fourier transformation to derive dispersion relation. For nonlinear analysis, we apply reductive perturbation method to derive Korteweg de Vries equation (KdV). The effects of variations of Coriolis force, spin polarization, and quantum parameter on characteristics of solitary structure are discussed. These results are applicable to astrophysical and laboratory plasmas.

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Precession as a probe of the neutron star interior

Link

2007

Isolated Neutron Stars: From the Surface to the Interior

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Postglitch behavior of the plasma inside neutron stars

Cited by 60 publications

References 0 publications

Short-Period Pulsar Oscillations Following a Glitch

Short-Period Pulsar Oscillations Following a Glitch

Spin density polarization effects in the presence of Coriolis force on ion acoustic waves in quantum plasma

Precession as a probe of the neutron star interior

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