Instabilities of current-sheet with a nonuniform guide field

Huang, Feng; Xu, Jinrong; Yan, Fei; Zhang, Min; Yu, M. Y.

doi:10.1063/1.4998481

Cited by 2 publications

(3 citation statements)

References 27 publications

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“…A similar, albeit not totally identical magnetic field profile has previously been used by Huang et al (2017) to study instabilities using this type of collisionless current sheet. We will show that this magnetic field profile can be used to consistently describe a transition from the Harris sheet to the force-free Harris sheet.…”

Section: Alternative Intermediate Casesmentioning

confidence: 96%

A family of Vlasov–Maxwell equilibrium distribution functions describing a transition from the Harris sheet to the force-free Harris sheet

2020

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We discuss a family of Vlasov–Maxwell equilibrium distribution functions for current sheet equilibria that are intermediate cases between the Harris sheet and the force-free (or modified) Harris sheet. These equilibrium distribution functions have potential applications to space and astrophysical plasmas. The existence of these distribution functions had been briefly discussed by Harrison & Neukirch (Phys. Rev. Lett., vol. 102, (2009a), 135003), but here it is shown that their approach runs into problems in the limit where the guide field goes to zero. The nature of this problem will be discussed and an alternative approach will be suggested that avoids the problem. This is achieved by considering a slight variation of the magnetic field profile, which allows a smooth transition between the Harris and force-free Harris sheet cases.

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Section: Alternative Intermediate Casesmentioning

confidence: 96%

A family of Vlasov–Maxwell equilibrium distribution functions describing a transition from the Harris sheet to the force-free Harris sheet

2020

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“…(where B is the magnetic field, j is the current density, and µ 0 is the permeability of free space) are thought to form in the solar atmosphere and planetary magnetospheres and are, therefore, often used for modelling purposes (e.g. Bobrova & Syrovatskiǐ 1979;Kivelson & Khurana 1995;Marsh 1996;Tassi, Pegoraro & Cicogna 2008;Wiegelmann & Sakurai 2012;Priest 2014;Akcay et al 2016;Burgess, Gingell & Matteini 2016;Borissov et al 2017;Gingell et al 2017;Huang et al 2017;Lukin et al 2018). Equations (1.1)-(1.3) imply that B and j are parallel to each other, i.e.…”

Section: Introductionmentioning

confidence: 99%

“…are thought to form in the solar atmosphere and planetary magnetospheres and are, therefore, often used for modelling purposes (e.g. Bobrova & Syrovatskiǐ (1979); Kivelson & Khurana (1995); Marsh (1996); Tassi et al (2008); Wiegelmann & Sakurai (2012); Priest (2014); Akcay et al (2016); Burgess et al (2016); Gingell et al (2017); Borissov et al (2017); Huang et al (2017); Lukin et al (2018)). Equations (1.1)-(1.3) imply that the magnetic field, B, and the current density, j, are parallel to each other, i.e.…”

Section: Introductionmentioning

confidence: 99%

Collisionless distribution functions for force-free current sheets: using a pressure transformation to lower the plasma beta

2018

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So far, only one distribution function giving rise to a collisionless nonlinear force-free current sheet equilibrium allowing for a plasma beta less than one is known (Allanson et al. 2015(Allanson et al. , 2016a. This distribution function can only be expressed as an infinite series of Hermite functions with very slow convergence and this makes its practical use cumbersome. It is the purpose of this paper to present a general method that allows us to find distribution functions consisting of a finite number of terms (therefore easier to use in practice), but which still allow for current sheet equilibria that can, in principle, have an arbitrarily low plasma beta. The method involves using known solutions and transforming them into new solutions using transformations based on taking integer powers (N ) of one component of the pressure tensor. The plasma beta of the current sheet corresponding to the transformed distribution functions can then, in principle, have values as low as 1/N . We present the general form of the distribution functions for arbitrary N and then, as a specific example, discuss the case for N = 2 in detail.

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Instabilities of current-sheet with a nonuniform guide field

Cited by 2 publications

References 27 publications

A family of Vlasov–Maxwell equilibrium distribution functions describing a transition from the Harris sheet to the force-free Harris sheet

A family of Vlasov–Maxwell equilibrium distribution functions describing a transition from the Harris sheet to the force-free Harris sheet

Collisionless distribution functions for force-free current sheets: using a pressure transformation to lower the plasma beta

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