Reinterpretation of mirror modes as trains of slow magnetosonic solitons

Stasiewicz, K.

doi:10.1029/2004gl021282

Cited by 38 publications

(49 citation statements)

References 16 publications

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“…This region has been denoted as slow alfvenons in the nomenclature introduced recently by Stasiewicz and Ekeberg (2008). Mirror modes, as demonstrated earlier by Stasiewicz (2004a) and reconfirmed further in this paper, belong to a smaller area denoted as slow magnetosonic solitons. An additional red region of unstable waves in the right lower corner corresponds to inertial electron Alfvén wave structures (IEAW), and it would vanish if m e = 0 is set in Eq.…”

Section: Dispersive Nonlinear Waves In Anisotropic Plasmassupporting

confidence: 73%

“…In a simplified version, with constant anisotropy, a p , the model has been used to study soliton solutions, which compare well with Cluster measurements (Stasiewicz, 2004a(Stasiewicz, ,b, 2005a, and to study polarization of solitary waves (Mjølhus, 2006). To illustrate applicability of this technique we apply it to Cluster measurements made on 12 February 2005 in the magnetosheath on an inbound orbit in the Southern Hemisphere.…”

Section: Polybaric Pressure Equationsmentioning

confidence: 99%

“…However, the properties of "mirror structures" as observed by Cluster can be quantitatively explained by models showing that they represent propagating trains of slow magnetosonic solitons (Baumgärtel et al, 2003;Stasiewicz, 2004aStasiewicz, ,b, 2005a moving with speed of 0-30 km/s, well below the local Alfvén speed. Furthermore, a global model of mirror modes in the bow shock -magnetosheath -magnetopause system by Johnson and Cheng (1997) predicts propagation of these waves due to a combination of diamagnetic drift and the Doppler shift of frequency associated with plasma flow (Johnson and Cheng, 1997).…”

Section: Introductionmentioning

confidence: 99%

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Modelling of mirror mode structures as propagating slow magnetosonic solitons

Stasiewicz

Cheng

2009

Ann. Geophys.

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Abstract. Cluster measurements in the magnetosheath with spacecraft separations of 2000 km indicate that magnetic pulsations interpreted as mirror mode structures are not frozen in plasma flow, but do propagate with speeds of up to ∼50 km/s. Properties of these pulsations are shown to be consistent with propagating slow magnetosonic solitons. By using nonlinear two fluid theory we demonstrate that the well known classical mirror instability condition corresponds to a small subset in a continuum of exponentially varying solutions. With the measured plasma moments we have determined parameters of the polybaric pressure model in the region of occurrence of mirror type structures and applied it to numerical modelling of these structures. In individual cases we obtain excellent agreement between observed mirror mode structures and numerical solutions for magnetosonic solitons.

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Section: Dispersive Nonlinear Waves In Anisotropic Plasmassupporting

confidence: 73%

Section: Polybaric Pressure Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Modelling of mirror mode structures as propagating slow magnetosonic solitons

Stasiewicz

Cheng

2009

Ann. Geophys.

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“…The multipoint measurements made it possible to provide all of the relevant parameters of the solitons and their environment for the first time. Stasiewicz (2004) applied a model of nonlinear waves in anisotropic plasmas, including electron inertial effects, to reinterpret mirror modes observed in the magnetosheath as trains of slow magnetosonic solitons. He obtained exact nonlinear magnetosonic wave-train solutions to the Hall-MHD equations with anisotropic ion pressure.…”

Section: Magnetosonic Solitonsmentioning

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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“…Recent development was stimulated by identification of magnetosonic solitons in Cluster measurements (Stasiewicz et al, 2003;Stasiewicz, 2004b), and modelling their properties with Hall-MHD equations integrated directly in the approach based on constants of motion (McKenzie et al, 2004), rather than on approximative DNSL solutions. Multi-fluid equations for bi-ion plasmas have oscillatory solutions with a soliton envelope, called "oscillitons" by Sauer et al (2001).…”

Section: Other Theoretical Models For Dispersive Alfvén Waves and Solmentioning

confidence: 99%

Dispersive MHD waves and alfvenons in charge non-neutral plasmas

Stasiewicz

Ekeberg

2008

Nonlin. Processes Geophys.

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Abstract. Dispersive properties of linear and nonlinear MHD waves, including shear, kinetic, electron inertial Alfvén, and slow and fast magnetosonic waves are analyzed using both analytical expansions and a novel technique of dispersion diagrams. The analysis is extended to explicitly include space charge effects in non-neutral plasmas. Nonlinear soliton solutions, here called alfvenons, are found to represent either convergent or divergent electric field structures with electric potentials and spatial dimensions similar to those observed by satellites in auroral regions. Similar solitary structures are postulated to be created in the solar corona, where fast alfvenons can provide acceleration of electrons to hundreds of keV during flares. Slow alfvenons driven by chromospheric convection produce positive potentials that can account for the acceleration of solar wind ions to 300-800 km/s. New results are discussed in the context of observations and other theoretical models for nonlinear Alfvén waves in space plasmas.

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Reinterpretation of mirror modes as trains of slow magnetosonic solitons

Cited by 38 publications

References 16 publications

Modelling of mirror mode structures as propagating slow magnetosonic solitons

Modelling of mirror mode structures as propagating slow magnetosonic solitons

Multipoint observations of plasma phenomena made in space by Cluster

Dispersive MHD waves and alfvenons in charge non-neutral plasmas

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