Neutron Star Magnetic Field Evolution, Crust Movement, and Glitches

Ruderman, M.; Zhu, T.; Chen, Kaiyou

doi:10.1086/305026

Cited by 274 publications

(350 citation statements)

References 44 publications

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“…But the magnitude and frequency of the Vela glitches could not be explained by this model, and a picture involving the sudden unpinning from the inner crust of superÑuid vortices in the core of the star became the dominant paradigm (Anderson & Itoh 1975). Observations of the relaxation of the star back toward its original spin-down rate suggest that D1% of the starÏs mass is involved in the event (Alpar et al 1988 ;Ruderman, Zhu, & Chen 1998), implying a total energy release of D1042 ergs.…”

Section: T Hermal Emission Constraints On the Neutronmentioning

confidence: 95%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

289

305

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We present high-resolution Chandra X-ray observations of PSR B0833[45, the 89 ms pulsar associated with the Vela supernova remnant. We have acquired two observations separated by 1 month to search for changes in the pulsar and its environment following an extreme glitch in its rotation frequency. We Ðnd a well-resolved nebula with a toroidal morphology remarkably similar to that observed in the Crab Nebula, along with an axial Crab-like jet. Between the two observations, taken D3 ] 105 s and D3 ] 106 s after the glitch, the Ñux from the pulsar is found to be steady to within 0.75% ; the 3 p limit on the fractional increase in the pulsarÏs X-ray Ñux is of the inferred glitch energy. We use [10~5 this limit to constrain parameters of glitch models and neutron star structure. We do Ðnd a signiÐcant increase in the Ñux of the nebulaÏs outer arc ; if associated with the glitch, the inferred propagation velocity is similar to that seen in the brightening of the Crab Nebula wisps. We propose an explana-Z0.7c, tion for the X-ray structure of the Vela synchrotron nebula based on a model originally developed for the Crab Nebula. In this model, the bright X-ray arcs are the shocked termination of a relativistic equatorial pulsar wind that is contained within the surrounding kidney-bean shaped synchrotron nebula comprising the postshock, but still relativistic, Ñow. In a departure from the Crab model, the magnetization parameter p of the Vela pulsar wind is allowed to be of order unity ; this is consistent with the simplest MHD transport of magnetic Ðeld from the pulsar to the nebula, where B ¹ 4 ] 10~4 G. The inclination angle of the axis of the equatorial torus with respect to the line of sight is identical to that of the rotation axis of the pulsar as previously measured from the polarization of the radio pulse. The projection of the rotation axis on the sky may also be close to the direction of proper motion of the pulsar if previous radio measurements were confused by orthogonal-mode polarized components. We review e †ects that may enhance the probability of alignment between the spin axis and space velocity of a pulsar, and speculate that short-period, slowly moving pulsars are just the ones best-suited to producing synchrotron nebulae with such aligned structures. Previous interpretations of the compact Vela nebula as a bow-shock in a very weakly magnetized wind su †ered from data of inadequate spatial resolution and less plausible physical assumptions.

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Section: T Hermal Emission Constraints On the Neutronmentioning

confidence: 95%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

289

305

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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%

“…For this reason, our force balance (51) does not include a 'pinning' force, resulting from the magnetic short-range interaction between the two arrays (Ruderman, Zhu & Chen 1998;Jahan-Miri 2000;Link 2003;. Calculating repeated cross products of the force balance equation withκ i p , pointing along the local orientation of a fluxtube, it is possible to express the mesoscopic fluxtube velocity in terms of the averaged fluid velocities,…”

Section: The Coupling Force: 'Standard' Resistivitymentioning

confidence: 99%

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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“…Despite recent advances in combining the microphysics and hydrodynamics of this model (Sidery et al 2010;van Eysden & Melatos 2010;Haskell et al 2012;Pizzochero 2011;Seveso et al 2012) certain aspects of the model such as the exact unpinning trigger and a convincing account of the process by which a large number of vortices subsequently moves remain to be addressed (Link & Epstein 1996;Glampedakis & Andersson 2009;Warszawski & Melatos 2008;Melatos & Warszawski 2009;Warszawski & Melatos 2013;Warszawski et al 2012). In addition, it is possible that pinning of neutron vortices occurs elsewhere in the star (Srinivasan et al 1990;Jones 1991;Mendell 1991;Ruderman et al 1998;Link 2003Link , 2012, or that at least some glitches arise by other means such as hydrodynamical instabilities and turbulence (Melatos & Peralta 2007;Andersson et al 2004).…”

Section: Introductionmentioning

confidence: 99%

Efficacy of crustal superfluid neutrons in pulsar glitch models

Hooker¹,

Newton²,

Li³

2015

Monthly Notices of the Royal Astronomical Society

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In order to assess the ability of purely crust-driven glitch models to match the observed glitch activity in the Vela pulsar, we conduct a systematic analysis of the dependence of the fractional moment of inertia of the inner crustal neutrons on the stiffness of the nuclear symmetry energy at saturation density L. We take into account both crustal entrainment and the fact that only a fraction Y g of the core neutrons may couple to the crust on the glitch-rise timescale. We use a set of consistently-generated crust and core compositions and equations-of-state which are fit to results of lowdensity pure neutron matter calculations. When entrainment is included at the level suggested by recent microscopic calculations and the core is fully coupled to the crust, the model is only able to account for the Vela glitch activity for a 1.4M star if the equation of state is particularly stiff L > 100 MeV. However, an uncertainty of about 10% in the crust-core transition density and pressure allows for the Vela glitch activity to be marginally accounted for in the range L ≈ 30 − 60MeV consistent with a range of experimental results. Alternatively, only a small amount of core neutrons need be involved. If less than 50% of the core neutrons are coupled to the crust during the glitch, we can also account for the Vela glitch activity using crustal neutrons alone for EOSs consistent with the inferred range of L. We also explore the possibility of Vela being a high-mass neutron star, and of crustal entrainment being reduced or enhanced relative to its currently predicted values.

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Neutron Star Magnetic Field Evolution, Crust Movement, and Glitches

Cited by 274 publications

References 44 publications

Vela Pulsar and Its Synchrotron Nebula

Vela Pulsar and Its Synchrotron Nebula

Magnetic field evolution in superconducting neutron stars

Efficacy of crustal superfluid neutrons in pulsar glitch models

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