Magnetic field amplification in newly-born neutron stars

Wiebicke, H.J.; Geppert, U.

doi:10.1017/s0252921100042056

Cited by 13 publications

(19 citation statements)

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“…Gradual field generation due to a thermomagnetic effect in the crust has been discussed (Urpin & Yakovlev 1980;Blandford et al 1983;Wiebicke & Geppert 1996), but it seems unlikely to be capable of producing large-scale fields stronger than 10 12 G.…”

Section: Origin Of Neutron Star Magnetic Fieldmentioning

confidence: 99%

Physics of strongly magnetized neutron stars

Harding¹,

Lai²

2006

Rep. Prog. Phys.

811

763

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Abstract. There has recently been growing evidence for the existence of neutron stars possessing magnetic fields with strengths that exceed the quantum critical field strength of 4.4 × 10 13 G, at which the cyclotron energy equals the electron rest mass. Such evidence has been provided by new discoveries of radio pulsars having very high spin-down rates and by observations of bursting gamma-ray sources termed magnetars. This article will discuss the exotic physics of this high-field regime, where a new array of processes becomes possible and even dominant, and where familiar processes acquire unusual properties. We review the physical processes that are important in neutron star interiors and magnetospheres, including the behavior of free particles, atoms, molecules, plasma and condensed matter in strong magnetic fields, photon propagation in magnetized plasmas, free-particle radiative processes, the physics of neutron star interiors, and field evolution and decay mechanisms. Application of such processes in astrophysical source models, including rotation-powered pulsars, soft gamma-ray repeaters, anomalous X-ray pulsars and accreting X-ray pulsars will also be discussed. Throughout this review, we will highlight the observational signatures of high magnetic field processes, as well as the theoretical issues that remain to be understood.

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Section: Origin Of Neutron Star Magnetic Fieldmentioning

confidence: 99%

Physics of strongly magnetized neutron stars

Harding¹,

Lai²

2006

Rep. Prog. Phys.

811

763

View full text Add to dashboard Cite

show abstract

“…The arguments on generation of magnetic field by the thermoelectric effects in the conducting crust of the neutron star with the immense gradient of temperature were extensively studied in papers 14,15,16 . Since there is uncertainty in microphysics of neutron stars we decided do not provide here any evaluation for magnetic flux (36) for this toy model.…”

Section: Magnetic Flux Through Superconducting Ring Inside a Rotatingmentioning

confidence: 99%

Electromagnetic Effects in Superconductors in Stationary Gravitational Field

Ahmedov

Kagramanova

2005

Int. J. Mod. Phys. D

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The general relativistic modifications to the resistive state in superconductors of second type in the presence of a stationary gravitational field are studied. Some superconducting devices that can measure the gravitational field by its red-shift effect on the frequency of radiation are suggested. It has been shown that by varying the orientation of a superconductor with respect to the earth gravitational field, a corresponding varying contribution to AC Josephson frequency would be added by gravity. A magnetic flux (being proportional to angular velocity of rotation Ω) through a rotating hollow superconducting cylinder with the radial gradient of temperature ∇rT is theoretically predicted. The magnetic flux is assumed to be produced by the azimuthal current arising from Coriolis force effect on radial thermoelectric current. Finally the magnetic flux through the superconducting ring with radial heat flow located at the equatorial plane interior the rotating neutron star is calculated. In particular it has been shown that nonvanishing magnetic flux will be generated due to the general relativistic effect of dragging of inertial frames on the thermoelectric current.

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“…Also, when considering the thermomagnetic field generation in the crust of young neutron stars (Wiebicke & Geppert 1996), where small-scale modes are the first ones to be excited, numerical instabilities occurred exclusively caused by the Hall-drift.…”

Section: Introductionmentioning

confidence: 99%

Non–linear magnetic field decay in neutron stars

Geppert

Rheinhardt

2002

A&A

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Abstract. There exists both theoretical and observational evidence that the magnetic field decay in neutron stars may proceed in a pronounced non-linear way during a certain episode of the neutron star's life. In the presence of a strong magnetic field the Hall-drift dominates the field evolution in the crust and/or the superfluid core of neutron stars. Analysing observations of P andṖ for sufficiently old isolated pulsars we gain strong hints for a significantly non-linear magnetic field decay. Under certain conditions with respect to the geometry and strength of a large-scale magnetic background field an instability is shown to occur which rapidly raises small-scale magnetic field modes. Their growth rates increase with the background field strength and may reach ∼10 4 times the ohmic decay rate. Consequences for the rotational and thermal evolution as well as for the cracking of the crust of neutron stars are discussed.

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Magnetic field amplification in newly-born neutron stars

Cited by 13 publications

References 1 publication

Physics of strongly magnetized neutron stars

Physics of strongly magnetized neutron stars

Electromagnetic Effects in Superconductors in Stationary Gravitational Field

Non–linear magnetic field decay in neutron stars

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