Magnetic structure of current sheets in magnetic fields with a singular X line

Bogdanov, S. Yu.; Bugrov, Sergey; Gritsyna, V. P.; Zverev, O. V.; Karpov, G. V.; Markov, V. S.; Repin, D. V.; Frank, A. G.

doi:10.1134/s1063780x07060013

Cited by 22 publications

(2 citation statements)

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“…The current J Z initiated 2D plasma flows in the magnetic field → B, and gave rise to the current sheet formation during the first 1-1.5 µs. The typical transverse sizes of the current sheet were: 2δx ≈ 12-17 cm (width) and 2δy ≈ 1.5-3.5 cm (thickness), at the level of 0.1 • j 0 z ; here, j 0 z is the current density at the middle plane of the sheet [27,28]. The sheet length along the direction of the current was equal to ∆z.…”

Section: Experimental Setup and Methods Of Diagnosticsmentioning

confidence: 99%

Characteristics of Plasma Dynamics in Current Sheets Formed in Helium Plasma

et al. 2021

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The characteristic features of plasma acceleration in the current sheets are discussed on the basis of an analysis of the structure of electrodynamic forces at successive stages of the evolution of the current sheets formed in the plasma with helium ions. Of particular interest is the generation of reverse currents at the side edges of the sheet and the appearance of forces, which are braking previously accelerated plasma flows.

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Section: Experimental Setup and Methods Of Diagnosticsmentioning

confidence: 99%

Characteristics of Plasma Dynamics in Current Sheets Formed in Helium Plasma

et al. 2021

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“…4 In geospace, global effects of reconnection are generally associated with X-points along separators (Dorelli et al 2007a,b), however, in the solar corona large amounts of stored energy appear to be released at magnetic nulls (see e.g., Antiochos et al 2002). Several regimes of non-ideal behavior and reconnection at magnetic null points have been hypothesized and modeled theoretically (Priest and Titov 1996;Pontin et al 2005;Parnell 2007;Priest and Pontin 2009;Wyper and Jain 2010;Galsgaard and Pontin 2011a,b;Pontin et al 2011), studied in the laboratory (Bogdanov et al 1994;Lukin and Linton 2011), and inferred from coronal observations (Parnell 2007;Parnell et al 2008).…”

Section: Plasma Phenomena As Measured In Three Dimensionsmentioning

confidence: 99%

Multipoint observations of plasma phenomena made in space by Cluster

et al. 2015

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Plasmas are ubiquitous in nature, surround our local geospace environment, and permeate the universe. Plasma phenomena in space give rise to energetic particles, the aurora, solar flares and coronal mass ejections, as well as many energetic phenomena in interstellar space. Although plasmas can be studied in laboratory settings, it is often difficult, if not impossible, to replicate the conditions (density, temperature, magnetic and electric fields, etc.) of space. Single-point space missions too numerous to list have described many properties of near-Earth and heliospheric plasmas as measured both in situ and remotely (see http://www.nasa.gov/missions/#.U1mcVmeweRY for a list of NASA-related missions). However, a full description of our plasma environment requires three-dimensional spatial measurements. Cluster is the first, and until data begin flowing from the Magnetospheric Multiscale Mission (MMS), the only mission designed to describe the three-dimensional spatial structure of plasma phenomena in geospace. In this paper, we concentrate on some of the many plasma phenomena that have been studied using data from Cluster. To date, there have been more than 2000 refereed papers published using Cluster data but in this paper we will, of necessity, refer to only a small fraction of the published work. We have focused on a few basic plasma phenomena, but, for example, have not dealt with most of the vast body of work describing dynamical phenomena in Earth's magnetosphere, including the dynamics of current sheets in Earth's magnetotail and the morphology of the dayside high latitude cusp. Several review articles and special publications are available that describe aspects of that research in detail and interested readers are referred to them (see for example, Escoubet et al.

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