Drift mirror instability in space plasmas, 2, Nonzero electron temperature effects

Pokhotelov, O. A.; Onishchenko, O. G.; Balikhin, M. A.; Treumann, R. A.; Павленко, В. Б.

doi:10.1029/2000ja000310

Cited by 24 publications

(43 citation statements)

References 32 publications

(12 reference statements)

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“…The effects of the suprathermal tails on the threshold conditions and the linear growth rates of these instabilities have widely been investigated in the last decade (Leubner and Schupfer, 2000Gedalin et al, 2001;Pokhotelov et al, 2002). A universal mirror wave-mode threshold condition for non-thermal space plasma environments was obtained by Leubner and Schupfer (2000.…”

Section: Anisotropic Kappa Distributionsmentioning

confidence: 97%

Kappa Distributions: Theory and Applications in Space Plasmas

Pierrard¹,

Lazar²

2010

Sol Phys

576

421

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The plasma particle velocity distributions observed in the solar wind generally show enhanced (non-Maxwellian) suprathermal tails, decreasing as a power law of the velocity and well described by the family of Kappa distribution functions. The presence of non-thermal populations at different altitudes in space plasmas suggests a universal mechanism for their creation and important consequences concerning plasma fluctuations, the resonant and nonresonant wave -particle acceleration and plasma heating. These effects are well described by the kinetic approaches where no closure requires the distributions to be nearly Maxwellian. This paper summarizes and analyzes the various theories proposed for the Kappa distributions and their valuable applications in coronal and space plasmas.

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Section: Anisotropic Kappa Distributionsmentioning

confidence: 97%

Kappa Distributions: Theory and Applications in Space Plasmas

Pierrard¹,

Lazar²

2010

Sol Phys

576

421

View full text Add to dashboard Cite

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“…The drift mirror instability also adheres to the same threshold conditions as the mirror instability. The convected mirror mode is a standing mode, while the drift mirror instability becomes oscillation with frequency equal to the particle drift wave frequency (Hasegawa, 1969;Pokhotelov et al, 2001;Rae et al, 2007). However, Hellinger (2008) pointed out that the threshold of the mirror instability, in the case of one cold species, is not applicable for the drift mirror instability.…”

Section: Introductionmentioning

confidence: 99%

Cluster and TC-1 observation of magnetic holes in the plasma sheet

Sun

Shi

et al. 2012

Ann. Geophys.

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Abstract. Magnetic holes with relatively small scale sizes, detected by Cluster and TC-1 in the magnetotail plasma sheet, are studied in this paper. It is found that these magnetic holes are spatial structures and they are not magnetic depressions generated by the flapping movement of the magnetotail current sheet. Most of the magnetic holes (93 %) were observed during intervals with B z larger than B x , i.e. they are more likely to occur in a dipolarized magnetic field topology. Our results also suggest that the occurrence of these magnetic holes might have a close relationship with the dipolarization process. The magnetic holes typically have a scale size comparable to the local proton Larmor radius and are accompanied by an electron energy flux enhancement at a 90 • pitch angle, which is quite different from the previously observed isotropic electron distributions inside magnetic holes in the plasma sheet. It is also shown that most of the magnetic holes occur in marginally mirror-stable environments. Whether the plasma sheet magnetic holes are generated by the mirror instability related to ions or not, however, is unknown. Comparison of ratios, scale sizes and propagation direction of magnetic holes detected by Cluster and TC-1, suggests that magnetic holes observed in the vicinity of the TC-1 orbit (∼7-12 R E ) are likely to be further developed than those observed by Cluster (∼7-18 R E ).

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“…The magnetic holes have been well studied in the solar wind [Stevens and Kasper, 2007, and references therein] and the magnetosheaths [Joy et al, 2006;Soucek et al, 2008, and references therein]. In the planetary magnetosheaths, the pressure anisotropy is generated as the plasma flow moves through the bow shock where the ion temperature increases with a larger proportion of heating preferentially going to the perpendicular component [Pokhotelov et al, 2001;Liu et al, 2005]. Close to the bow shock, mirror modes are generated and appear as quasi-sinusoidal waves in the early stages of development.…”

Section: Introductionmentioning

confidence: 99%

Case studies of mirror-mode structures observed by THEMIS in the near-Earth tail during substorms

et al. 2011

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[1] An examination of the magnetic field and plasma observed by the inner THEMIS-D spacecraft (P3) close to the equatorial plane at ∼11R E at local midnight reveals the occurrence of mirror-mode structures. These structures have the same characteristic waveform seen in other regions. The examination of the mirror-mode instability shows that inside these structures the threshold of mirror instability is marginally reached, while the surrounding plasma is mirror stable. The observed mirror structures occur in the dipolarized magnetic field following a substorm-related dipolarization. It is found that after the dipolarization front, the local ions become more anisotropic and initial magnetic holes form inside this anisotropic plasma before the fully-fledged mirror structures are observed. The ions become less anisotropic afterward, but the strong field depression in the magnetic holes enhances the effective plasma beta so that the mirror instability threshold is marginally reached. Thus, the dipolarization process provides the large-amplitude magnetic field fluctuations and the anisotropic plasma environment for mirror structures to grow. The isolated large-amplitude mirror-mode structures survive in the mirror-stable plasma even through the plasma becomes less anisotropic. It is also found that the width of magnetotail mirror-structures is smaller than one gyroradius of a plasma sheet proton, which is different from the width of mirror structures in other regions. These mirror structures appear to have a strong correlation with electron anisotropy changes. These observations suggest that electron kinetics may also play a role during the growth and saturation of mirror instability in the near-Earth tail.

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Drift mirror instability in space plasmas, 2, Nonzero electron temperature effects

Cited by 24 publications

References 32 publications

Kappa Distributions: Theory and Applications in Space Plasmas

Kappa Distributions: Theory and Applications in Space Plasmas

Cluster and TC-1 observation of magnetic holes in the plasma sheet

Case studies of mirror-mode structures observed by THEMIS in the near-Earth tail during substorms

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