Rapid postglitch spin-up of the superfluid core in pulsars

Alpar, M. A.; Langer, Stephen A.; Sauls, J. A.

doi:10.1086/162232

Cited by 353 publications

(584 citation statements)

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“…Due to the multi-fluid nature of the superfluid/superconducting mixture, there are not simply two components coupled by a single resistive force. We could imagine a variety of ways for the components to interact with each other ranging from electron scattering (Sauls, Stein & Serene 1982;Alpar, Langer & Sauls 1984;Andersson, Sidery & Comer 2006) and vortexfluxtube interactions (Ruderman, Zhu & Chen 1998;Jahan-Miri 2000;Link 2003) to shear or bulk viscosity (Andersson, Comer & Glampedakis 2005;Shternin & Yakovlev 2008;Manuel, Tarrus & Tolos 2013). Choosing a more pedagogical approach to our problem, we pick one specific mechanism, determine how it affects the electrons on mesoscopic scales and translate this into a macroscopic picture.…”

Section: The Coupling Force: 'Standard' Resistivitymentioning

confidence: 99%

“…We, therefore, consider the scattering of electrons off the vortex/fluxtube magnetic fields as a source of mutual friction. This 'standard' resistive coupling in a superfluid/superconducting mixture, first discussed by Alpar, Langer & Sauls (1984), results in two forces acting on the electrons,…”

Section: The Coupling Force: 'Standard' Resistivitymentioning

confidence: 99%

“…In Section 3, the standard resistive MHD formalism is reviewed. We then discuss the case of superconducting matter in Section 4, focussing on the standard resistive coupling introduced by Alpar, Langer & Sauls (1984). After giving the most general form of the superconducting induction equation, we use a few assumptions to simplify and interpret our results.…”

Section: Introductionmentioning

confidence: 99%

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Magnetic field evolution in superconducting neutron stars

Graber

Andersson

Glampedakis

et al. 2015

Mon. Not. R. Astron. Soc.

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The presence of superconducting and superfluid components in the core of mature neutron stars calls for the rethinking of a number of key magnetohydrodynamical notions like resistivity, the induction equation, magnetic energy and flux-freezing. Using a multi-fluid magnetohydrodynamics formalism, we investigate how the magnetic field evolution is modified when neutron star matter is composed of superfluid neutrons, type-II superconducting protons and relativistic electrons. As an application of this framework, we derive an induction equation where the resistive coupling originates from the mutual friction between the electrons and the vortex/fluxtube arrays of the neutron and proton condensates. The resulting induction equation allows the identification of two timescales that are significantly different from those of standard magnetohydrodynamics. The astrophysical implications of these results are briefly discussed.

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Section: The Coupling Force: 'Standard' Resistivitymentioning

confidence: 99%

Section: The Coupling Force: 'Standard' Resistivitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Magnetic field evolution in superconducting neutron stars

Graber

Andersson

Glampedakis

et al. 2015

Mon. Not. R. Astron. Soc.

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“…A two fluid model of neutron star cores, of the kind that is commonly used in hydrodynamical simulations has been developed in the past, assuming a neutron-proton-electron composition and using a non relativistic treatment, by the work of many authors [1,2]. In particular, as explained by Borumand et al [3], appropriate expressions have been obtained for the relevant entrainment coefficients, relating the momentum of the neutron fluid to the particle current of both neutrons and protons, in terms of the Landau parameters in the Fermi liquid theory.…”

Section: Introductionmentioning

confidence: 99%

Effect of BCS pairing on entrainment in neutron superfluid current in neutron star crust

2005

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“…The bulk of superconducting protons do not rotate by forming vortices, which differs from neutron superfluid. Superconducting protons corotate with the crust and electron fluid by generating a surface current that produces a small uniform magnetic field in the interior H ¼ À2m p c =e, where m p and e are the proton mass and charge, respectively (Alpar, Langer, & Sauls 1984). The vector potential associated with this field A ¼ Àm p cðX µ rÞ=e yields the proton velocity that corresponds to rigid body rotation…”

Section: Magnetic Field Associated With Neutron Vorticesmentioning

confidence: 99%

Radiation of Neutron Stars Produced by Superfluid Core

Svidzinsky

2003

ApJ

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We find a new mechanism of neutron star radiation wherein radiation is produced by the stellar interior. The main finding is that the neutron star interior is transparent for collisionless electron sound, the same way as it is transparent for neutrinos. In the presence of the magnetic field the electron sound is coupled with electromagnetic radiation; such collective excitation is known as a fast magnetosonic wave. At high densities such waves reduce to the zero sound in electron liquid, while near the stellar surface they are similar to electromagnetic waves in a medium. We find that zero sound is generated by superfluid vortices in the stellar core. Thermally excited helical vortex waves produce fast magnetosonic waves in the stellar crust that propagate toward the surface and transform into outgoing electromagnetic radiation. The magnetosonic waves are partially absorbed in a thin layer below the surface. The absorption is highly anisotropic; it is smaller for waves that in the absorbing layer propagate closer to the magnetic field direction. As a result, the vortex radiation is pulsed with the period of star rotation. The vortex radiation has the spectral index % À0:45 and can explain nonthermal radiation of middle-aged pulsars observed in the infrared, optical, and hard X-ray bands. The radiation is produced in the star interior, rather than in the magnetosphere, which allows direct determination of the core temperature. Comparing the theory with available spectra observations, we find that the core temperature of the Vela pulsar is T % 8 Â 10 8 K, while the core temperature of PSR B0656+14 and Geminga exceeds 2 Â 10 8 K. This is the first measurement of the temperature of a neutron star core. The temperature estimate rules out equations of state incorporating Bose condensations of pions or kaons and quark matter in these objects. The estimate also allows us to determine the critical temperature of triplet neutron superfluidity in the Vela core, T c ¼ ð7:5 AE 1:5Þ Â 10 9 K, which agrees well with the value of critical temperature in a core of a canonical neutron star calculated based on recent data for behavior of strong interactions at high energies. We also find that in the middle-aged neutron stars the vortex radiation, rather than thermal conductivity, is the main mechanism of heat transfer from the stellar core to the surface. The core radiation opens a possibility to study composition of neutron star crust by detection of absorption lines corresponding to the low-energy excitations of crust nuclei. Bottom layers of the crust may contain exotic nuclei with the mass number up to 600, and the core radiation creates a perspective to study their properties. In principle, zero sound can also be emitted by other mechanisms, rather than vortices. In this case the spectrum of stellar radiation would contain features corresponding to such processes. As a result, zero sound opens a perspective of direct spectroscopic study of superdense matter in the neutron star interior.

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Rapid postglitch spin-up of the superfluid core in pulsars

Cited by 353 publications

References 0 publications

Magnetic field evolution in superconducting neutron stars

Magnetic field evolution in superconducting neutron stars

Effect of BCS pairing on entrainment in neutron superfluid current in neutron star crust

Radiation of Neutron Stars Produced by Superfluid Core

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