The Hall effect and oscillating decay of a magnetic field

Shalybkov, D. A.; Урпин, В. А.

doi:10.1134/1.1259587

Cited by 62 publications

(89 citation statements)

References 3 publications

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“…During the last two decades, many authors have studied the effects of Hall drift onto the evolution of magnetic fields in isolated NSs (Haensel et al 1990;Goldreich & Reisenegger 1992;Muslimov 1994;Naito & Kojima 1994;Urpin & Shalybkov 1995;Shalybkov & Urpin 1997;Vainshtein et al 2000;Hollerbach & Ruediger 2002;Geppert et al 2003;Rheinhardt et al 2004;Cumming et al 2004). By use of the analogy of the Hall induction equation with the vorticity equation of an incompressible liquid, Goldreich & Reisenegger (1992) developed the idea of the Hall cascade.…”

Section: Introductionmentioning

confidence: 99%

Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars

Pons¹,

Geppert²

2007

A&A

203

253

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Context. We study the non-linear evolution of magnetic fields in neutron star crusts with special attention to the influence of the Hall drift. Aims. Our goal is to understand the conditions for fast dissipation due to the Hall term in the induction equation. We study the interplay of Ohmic dissipation and Hall drift in order to find a timescale for the overall crustal field decay. Methods. We solve numerically the Hall induction equation by means of a hybrid method (spectral in angles but finite differences in the radial coordinate). The microphysical input consists of the most modern available crustal equation of state, composition and electrical conductivities.Results. We present the first long term simulations of the non-linear magnetic field evolution in realistic neutron star crusts with a stratified electron number density and temperature dependent conductivity. We show that Hall drift influenced Ohmic dissipation takes place in neutron star crusts on a timescale of 10 6 years. When the initial magnetic field has magnetar strength, the fast Hall drift results in an initial rapid dissipation stage that lasts ∼ 10 4 years. The interplay of the Hall drift with the temporal variation and spatial gradient of conductivity tends to favor the displacement of toroidal fields toward the inner crust, where stable configurations can last for ∼ 10 6 years. We show that the thermally emitting isolated neutron stars, as the Magnificent Seven, are very likely descendants of neutron stars born as magnetars.

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Section: Introductionmentioning

confidence: 99%

Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars

Pons¹,

Geppert²

2007

A&A

203

253

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“…Here, we intend to consider as the non-linearity of the field evolution the Hall-effect or Hall-drift, as it occurs in the crust (see, e.g., Shalybkov & Urpin 1997), i.e., both ambipolar diffusion and any convective motion of the neutron star matter is excluded.…”

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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“…It has a profound influence, for instance, on the magnetic field dynamics in dense molecular clouds (Wardle & Ng 1999), and in accretion disks (especially in protostellar disks) it strongly affects the Balbus-Hawley magnetorotational instability (Wardle 1999;Balbus & Terquem 2001). Norman & Heyvaerts (1985) also noted that the Hall effect may become significant during star formation, and its relevance to compact objects such as white dwarfs and neutron stars (Urpin & Yakovlev 1980;Shalybkov & Urpin 1997;Potekhin 1999) has also been discussed. In addition, it can play a crucial role in the generation and evolution of magnetic fields in the early universe (Tajima et al 1992).…”

Section: Introductionmentioning

confidence: 99%

Dynamo Action in Magnetohydrodynamics and Hall‐Magnetohydrodynamics

Mininni

Gomez

Mahajan

2003

ApJ

128

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The first direct numerical simulations of turbulent Hall dynamos are presented. The evolution of an initially weak and small-scale magnetic field in a system maintained in a stationary regime of hydrodynamic turbulence (by a stirring force at a macroscopic scale) is studied to explore the conditions for exponential growth of the magnetic energy. The Hall current is shown to have a profound effect on turbulent dynamo action; it can strongly enhance or suppress the generation of the large-scale magnetic energy depending on the relative values of the length scales of the system.

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The Hall effect and oscillating decay of a magnetic field

Cited by 62 publications

References 3 publications

Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars

Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars

Non–linear magnetic field decay in neutron stars

Dynamo Action in Magnetohydrodynamics and Hall‐Magnetohydrodynamics

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