Some features of the plasma flow in the magnetosheath behind quasi-parallel and quasi-perpendicular bow shocks

Shevyrev, N. N.; Zastenker, G. N.

doi:10.1016/j.pss.2004.09.033

Cited by 68 publications

(57 citation statements)

References 16 publications

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“…A similar finding follows from the papers by Shevyrev and Zastenker (2005); Shevyrev et al (2007). These authors concluded that in the magnetosheath, the plasma flow is mainly turbulent and that the character of the turbulence is strongly controlled by the θ BN angle.…”

Section: The Importance Of the Magnetosheath Lies In The Fact That Itsupporting

confidence: 84%

Correlation length of magnetosheath fluctuations: Cluster statistics

2008

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Abstract. Magnetosheath parameters are usually described by gasdynamic or magnetohydrodynamic (MHD) models but these models cannot account for one of the most important sources of magnetosheath fluctuations -the foreshock. Earlier statistical processing of a large amount of magnetosheath observations has shown that the magnetosheath magnetic field and plasma flow fluctuations downstream of the quasiparallel shock are much larger than those at the opposite flank. These studies were based on the observations of a single spacecraft and thus they could not provide full information on propagation of the fluctuations through the magnetosheath.We present the results of a statistical survey of the magnetosheath magnetic field fluctuations using two years of Cluster observations. We discuss the dependence of the crosscorrelation coefficients between different spacecraft pairs on the orientation of the separation vector with respect to the average magnetic field and plasma flow vectors and other parameters. We have found that the correlation length does not exceed ∼1 R E in the analyzed frequency range (0.001-0.125 Hz) and does not depend significantly on the magnetic field or plasma flow direction. A close connection of crosscorrelation coefficients computed in the magnetosheath with the cross-correlation coefficients between a solar wind monitor and a magnetosheath spacecraft suggests that solar wind structures persist on the background of magnetosheath fluctuations.

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Section: The Importance Of the Magnetosheath Lies In The Fact That Itsupporting

confidence: 84%

Correlation length of magnetosheath fluctuations: Cluster statistics

2008

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“…In this study, due to the limited statistics (limited number of crossings the magnetopause by one of the spacecrafts, when the other was performing measurements upstream the foreshock region) we does not distinguish events with quasiperpendicular and quasiparallel shock waves. In accordance with the results of Shevyrev and Zastenker (2005) one can expect that the average level of fluctuations behind quasiperpendicular and quasiparallel shock waves will differ by about a factor of 2.…”

Section: Conclusion and Discussionsupporting

confidence: 85%

“…The magnetosheath is a region through which mass, energy and momentum are transported from the solar wind into the Earth's magnetosphere. There is a significant number of experimental results showing the high level of plasma turbulence in the magnetosheath (see Luhmann et al (1986), Sibeck et al (2000), Zastenker et al (1999Zastenker et al ( , 2002, Lucek et al (2001), Nĕmeček et al (2000a,b;2002a,b), Shevyrev & Zastenker (2005), Shevyrev et al (2007), Gutynska et al (2008), Savin et al (2008), Rossolenko et al (2008), Ŝafránková et al (2009Ŝafránková et al ( ), Znatkova et al (2011 and references therein). Fig.…”

Section: Turbulent Magnetosheath and Magnetic Field Near The Subsolarmentioning

confidence: 99%

Turbulence in the Magnetosheath and the Problem of Plasma Penetration Inside the Magnetosphere

Антонова¹,

Pulinets²,

Рязанцева³

et al. 2012

Exploring the Solar Wind

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“…It is important to note, however, that monochromatic AIC and mirror modes, visible in Fourier spectrum as sharp peaks (see for example (Alexandrova et al, 2004)), are not frequently seen in the magnetosheath. Instead, most of the observations shows a broad band spectrum covering frequencies much higher than f ci (Siscoe et al, 1967;Rezeau et al, 1986Rezeau et al, , 1999Rezeau et al, , 2001Matsuoka et al, 2000;Shevyrev and Zastenker, 2005;Sahraoui et al, 2003aSahraoui et al, , 2006. Let us discuss more in details some features of magnetic fluctuations below and above f ci .…”

Section: The Earth Magnetosheathmentioning

confidence: 99%

Solar wind vs magnetosheath turbulence and Alfvén vortices

Alexandrova

2008

Nonlin. Processes Geophys.

112

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Abstract. In this paper we give firstly a broad review of the space plasma turbulence around the ion characteristic space and temporal scales within two natural laboratories, the solar wind and the Earth magnetosheath. In both regions power law spectra of magnetic fluctuations are observed. In both regions these spectra have a break in the vicinity of the ion cyclotron frequency. A distinctive feature of the magnetosheath turbulence is the presence of Alfvén vortices at scales of the spectral break. The Alfvén vortices are multi-scale nonlinear structures. We give a review of the main theoretical features of incompressible Alfvén vortsices in the second part of the paper. Finally, we analyze the spectral properties of the Alfvén vortex solution and of the network of such vortices. We show that the observed magnetosheath spectrum in presence of the Alfvén vortices can be described, at least partially, by the vortex network model.

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Some features of the plasma flow in the magnetosheath behind quasi-parallel and quasi-perpendicular bow shocks

Cited by 68 publications

References 16 publications

Correlation length of magnetosheath fluctuations: Cluster statistics

Correlation length of magnetosheath fluctuations: Cluster statistics

Turbulence in the Magnetosheath and the Problem of Plasma Penetration Inside the Magnetosphere

Solar wind vs magnetosheath turbulence and Alfvén vortices

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