One-Dimensional Vlasov-Maxwell Equilibrium for the Force-Free Harris Sheet

Harrison, M.; Neukirch, T.

doi:10.1103/physrevlett.102.135003

Cited by 69 publications

(162 citation statements)

References 19 publications

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“…Recently the first nonlinear force-free, non-relativistic VM equilibrium for the force-free Harris sheet was reported by Harrison and Neukirch 9 . If the thermal energy of the plasma approaches or exceeds its rest energy, a non-relativistic treatment is no longer sufficient and a relativistic analogue must be sought.…”

Section: Discussionmentioning

confidence: 99%

“…This paper has presented a collisionless distribution function for the relativistic force-free Harris sheet. Mirroring the non-relativistic solution [9][10][11] , where the properties of the pressure tensor were exploited, the energy-momentum tensor T αβ was wielded in an equivalent role 27 , allowing the calculation of the equilibrium. In our Alternative methods of studying relativistic VM equilibria have also been developed [28][29][30][31][32][33][34] .…”

Section: Discussionmentioning

confidence: 99%

“…So far only a small number of one-dimensional (1D) collisionless force-free plasma equilibria is known, of which most belong to the class of linear force-free fields [4][5][6][7][8] . So far, analytical self-consistent distribution functions have been found only for one example of non-linear force-free fields, the force-free Harris sheet [9][10][11][12] . Finding self-consistent force-free collisionless equilibria is difficult, because one is dealing with an inverse problem, i.e.…”

Section: Introductionmentioning

confidence: 99%

“…In order to find the relativistic generalization of the collisionless distribution function for the force-free Harris sheet, we shall use the relativistic version [22][23][24] of the distribution function of the normal Harris sheet 25 as a guide, together with the non-relativistic distribution function for the force-free Harris sheet. 9,11 The paper is structured as follows: section II summarizes the mathematical framework of the non-relativistic force-free Harris sheet 9 . Section III then uses this as a basis for determining the distribution function for the relativistic force-free Harris sheet, and Section IV we present a discussion and our conclusions.…”

Section: Introductionmentioning

confidence: 99%

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Collisionless distribution function for the relativistic force-free Harris sheet

Stark

Neukirch

2012

Physics of Plasmas

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A self-consistent collisionless distribution function for the relativistic analogue of the force-free Harris sheet is presented. This distribution function is the relativistic generalization of the distribution function for the non-relativistic collisionless force-free Harris sheet recently found by Harrison and Neukirch [Phys. Rev. Lett. 102, 135003 (2009)] as it has the same dependence on the particle energy and canonical momenta.We present a detailed calculation which shows that the proposed distribution function generates the required current density profile (and thus magnetic field profile) in a frame of reference in which the electric potential vanishes identically. The connection between the parameters of the distribution function and the macroscopic parameters such as the current sheet thickness is discussed.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Collisionless distribution function for the relativistic force-free Harris sheet

Stark

Neukirch

2012

Physics of Plasmas

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“…For the method to work one has to ensure that 0 [3,31,32]) for all possible values of A x , A y . This imposes additional conditions which the parameters of the distribution function have to satisfy.…”

Section: Basic Theorymentioning

confidence: 99%

Collisionless current sheet equilibria

Neukirch

Wilson

Allanson

2017

Plasma Phys. Control. Fusion

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Current sheets are important for the structure and dynamics of many plasma systems. In space and astrophysical plasmas they play a crucial role in activity processes, for example by facilitating the release of magnetic energy via processes such as magnetic reconnection. In this contribution we will focus on collisionless plasma systems. A sensible first step in any investigation of physical processes involving current sheets is to find appropriate equilibrium solutions. The theory of collisionless plasma equilibria is well established, but over the past few years there has been a renewed interest in finding equilibrium distribution functions for collisionless current sheets with particular properties, for example for cases where the current density is parallel to the magnetic field (force-free current sheets). This interest is due to a combination of scientific curiosity and potential applications to space and astrophysical plasmas. In this paper we will give an overview of some of the recent developments, discuss their potential applications and address a number of open questions.

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Electron currents supporting the near‐Earth magnetotail during current sheet thinning

Artemyev

Angelopoulos

Liu

et al. 2017

Geophysical Research Letters

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Formation of intense, thin current sheets (i.e., current sheet thinning) is a critical process for magnetospheric substorms, but the kinetic physics of this process remains poorly understood. Using a triangular configuration of the three Time History of Events and Macroscale Interactions during Substorms (THEMIS) spacecraft at the end of 2015 we investigate field‐aligned and transverse currents in the magnetotail current sheet around 12 Earth radii downtail. Combining the curlometer technique with direct measurements of ion and electron velocities, we demonstrate that intense, thin current sheets supported by strong electron currents form in this region. Electron field‐aligned currents maximize near the neutral plane Bx∼0, attaining magnitudes of ∼20 nA/m2. Carried by hot (>1 keV) electrons, they generate strong magnetic shear, which contributes up to 20% of the vertical (along the normal direction to the equatorial plane) pressure balance. Electron transverse currents, on the other hand, are carried by the curvature drift of anisotropic, colder (<1 keV) electrons and gradually increase during the current sheet thinning. In the events under consideration the thinning process was abruptly terminated by earthward reconnection fronts which have been previously associated with tail reconnection further downtail. It is likely that the thin current sheet properties described herein are similar to conditions further downtail and are linked to the loss of stability and onset of reconnection there. Our findings are likely applicable to thin current sheets in other geophysical and astrophysical settings.

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One-Dimensional Vlasov-Maxwell Equilibrium for the Force-Free Harris Sheet

Cited by 69 publications

References 19 publications

Collisionless distribution function for the relativistic force-free Harris sheet

Collisionless distribution function for the relativistic force-free Harris sheet

Collisionless current sheet equilibria

Electron currents supporting the near‐Earth magnetotail during current sheet thinning

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