Wave properties in the magnetic reconnection diffusion region with high <i>β</i>: Application of the <i>k</i>‐filtering method to Cluster multispacecraft data

Huang, Suming; Zhou, Meng; Sahraoui, Fouad; Deng, X. H.; Pang, Y.; Yuan, Zhigang; Wei, Qianqian; Wang, J. F.; Zhou, Xiaomin

doi:10.1029/2010ja015335

Cited by 53 publications

(42 citation statements)

References 37 publications

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“…Observationally whistler waves have indeed been detected in magnetic reconnection regions in magnetosphere plasmas where the plasma beta is on the order of unity [27,32,33]. The wave was found obliquely propagated with its wavevector nearly perpendicular to the ambient magnetic field, in a good agreement with the dispersion relation (8) [27].…”

Section: Whistler Waves In the Reconnection Layersupporting

confidence: 70%

“…The wave was found obliquely propagated with its wavevector nearly perpendicular to the ambient magnetic field, in a good agreement with the dispersion relation (8) [27]. The exact formula of the dispersion relation (8) was further confirmed recently by k-filter analysis for Cluster observation data [33]. It was also observed that the polarity of the wave was right-handed in the plane perpendicular to the ambient magnetic field, a typical electron mode feature [27,32].…”

Section: Whistler Waves In the Reconnection Layersupporting

confidence: 61%

“…Analytical and numerical advances in collisionless magnetic reconnection based on Hall MHD and other similar models such as the hybrid model [16][17][18][19][20][21][22][23][24][25] have been largely driven by satellite observations in the last decade [26][27][28][29][30][31][32][33][34]. We in this paper review these developments and discuss outstanding issues raised by satellite observations and to be answered by theory and simulation.…”

Section: / 4πmentioning

confidence: 99%

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Recent progresses in theoretical studies and satellite observations for collisionless magnetic reconnection

Wang

Xiao

et al. 2012

Chin. Sci. Bull.

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As an essential mechanism in large scale fast magnetic energy releases and field reconfigurations processes in space, astrophysical, and laboratory plasmas, magnetic reconnection, particularly collisionless magnetic reconnection, has been studied for more than 65 years. Many progresses have been achieved in recent years and basic features of the process have been well understood, largely due to more and more satellite observation data available in the last decade. However, a few outstanding issues are still remained unresolved. We in the paper review the development of collisionless magnetic reconnection studies and major achievements in recent years, and also briefly discuss the open questions remained to be answered in studies of collisionless magnetic reconnection. Magnetic reconnection is thought an essential mechanism in many plasma physics processes in space, laboratory, and astrophysical objects, related to configurations relaxation and fast release of magnetic field and energy, observed in laboratory experiments and satellites observations and studied in numerical simulations and theoretical analysis [1]. The concept of magnetic reconnection was first proposed as a process of oppositely directed magnetic field lines merging and annihilated at a magnetic null, in an effort to understand the solar flare phenomenon It has then become a fundamental model in magnetic reconnection studies. Nevertheless, the Sweet-Parker reconnection rate is on the order of square root of the electrical resistivity. Due to the low collisionality in space and solar plasmas, the rate is too slow to be counted for fast events such as solar flares.Another model was then proposed by Petschek, with a fast driven and an X-point geometry, to solve the problem [5]. It was claimed in the Petschek model that a fast reconnection rate could be almost on the order of logarithm of resistivity, much faster than the Sweet-Parker rate. It was however found latterly that in high resolution simulations, the X-point geometry could not be realized in high Lundquist number regime of S≥10 4 [6]. And in the low Lundquist number regime (S<10 3 ), Petschek reconnection rate and Sweet-Parker reconnection rate would be more or less on the same order. On the other hand, collisionless mechanisms such as the finite Larmor radius (FLR) effect rather than collisional

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Section: Whistler Waves In the Reconnection Layersupporting

confidence: 70%

Section: Whistler Waves In the Reconnection Layersupporting

confidence: 61%

Section: / 4πmentioning

confidence: 99%

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Recent progresses in theoretical studies and satellite observations for collisionless magnetic reconnection

Wang

Xiao

et al. 2012

Chin. Sci. Bull.

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“…Magnetic reconnection in the terrestrial magnetosphere has been confirmed directly by in situ observations [1][2][3][4][5]. Recently, there were many observations of reconnection in the solar wind, which were often associated with interplanetary coronal mass ejection (ICME) [6][7][8].…”

mentioning

confidence: 78%

Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

et al. 2012

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Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy, and simultaneously changes the magnetic field topology. In this paper, we report the first observation of energetic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection. The magnetic field shear angle was about 151°, implying guide-field reconnection. The width of the exhaust was about 8×10 4 km. The reconnection rate was estimated as 0.044-0.08, which is consistent with fast reconnection theory and previous observations. We observed flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust. The region where energetic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere. We discuss these observation results, and compare with previous observations and recent kinetic simulations.

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“…The method can be used on fully coupled electromagnetic wave time series provided the proper constraints (e.g., Faraday's Law) are in place (Tjulin et al 2005(Tjulin et al , 2008. P (ω, k), the main product of the k-filtering technique, has been used in a number of studies and in a number of different ways, including determining three-dimensional dispersion relations in identifying the plasma modes that characterize fluctuations in the magnetosheath (Glassmeier et al 2001;Sahraoui et al 2003Sahraoui et al , 2004, in the high latitude magnetic cusps (Grison et al 2005), in the magnetotail in conjunction with magnetic reconnection (Eastwood et al 2009;Huang et al 2010); and in the solar wind. Three-dimensional wavenumber spectra of turbulence have been produced by integrating over the angular frequencies P (k) = P (ω, k)dω in studies of lowfrequency magnetosheath turbulence (Sahraoui et al 2006), MHD-scale turbulence in the foreshock and solar wind (Narita et al 2006(Narita et al , 2010, and kinetic-scale turbulence in the solar wind (Sahraoui et al 2010b).…”

Section: Turbulencementioning

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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Wave properties in the magnetic reconnection diffusion region with high β: Application of the k‐filtering method to Cluster multispacecraft data

Cited by 53 publications

References 37 publications

Recent progresses in theoretical studies and satellite observations for collisionless magnetic reconnection

Recent progresses in theoretical studies and satellite observations for collisionless magnetic reconnection

Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

Multipoint observations of plasma phenomena made in space by Cluster

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