Resonant modes with frequencies 0.02–10 mHz are detected from the bow shock (BS) to the outer magnetosphere, with the nature of the resonances at frequencies 0.02–0.25 mHz being still unexplained. We propose a BS model in the form of a circular plate free along the outer edge that predicts resonant modes at frequencies 0.02–0.3 mHz or lower. We demonstrate the detection of these model resonant modes based on data from five satellites, with the resonance near 0.1 mHz predicted by the model being observed in the magnetosheath continuously for 17 hours downstream of both parallel and perpendicular shocks. Resonant BS modes produce three-wave nonlinear cascades that realize a broadband coherent coupling with resonances both near and inside the magnetopause. In our opinion, it is the coherent nature of the processes in an extended region with different linear resonant eigenmodes that determines the fairly new, nonlinear-cascade, approach to an efficient conversion of the energy of an inflow when interacting with an obstacle. This seems important for the entire nonlinear physics. We also provide arguments suggesting the possibility of resonant mode self-generation in the closed BS/magnetopause loop with a feedback in the form of narrow Poynting vector pulses at the cost of solar wind energy.

The linear and nonlinear resonances and cascades affecting significantly the interaction of a collisionless plasma flow with a magnetic barrier and the plasma penetration into the barrier are studied using the near-Earth magnetopause as an example. Our linear theory of the membrane instability of the boundary of a magnetic barrier, the magnetopause, explains the structure of the spectra and bi-spectra of fluctuations on different segments of the boundary layers near the magnetopause and the resonances at frequencies 0.05–0.5 mHz. The recorded compressibility of waves under the magnetopause implies that their excitation by Alfv’en resonances alone is impossible. We assume, as a general principle, an approximate coincidence of the frequencies of different harmonics of different resonances as a condition for the amplification of resonances to nonlinear amplitudes and their propagation into the ionosphere. We confirm the presence of resonant waves near the magnetopause and demonstrate a nonlinear three-wave cascade interaction of compressible (0.05–5 mHz) and incompressible waves under the magnetopause that provides the excitation of resonances of magnetic field lines and waveguide resonances at frequencies 1–25 mHz without a close coincidence of the frequencies with linear resonances at the magnetopause and the bow shock. This can also provide a nonlinear coupling of linear and nonlinear resonances in other multilayered media (for example, in the plasma and neutral sheets of the geomagnetic tail and between it and the magnetopause). An example of the excitation of a waveguide mode inside the magnetopause by nonlinear membrane waves is given. We have detected a nonlinear excitation and interaction of most “magic” harmonics under the magnetopause.

The theory of charged current sheets is compared with plasma data of Prognoz-8, Interball-1, Polar, and Cluster satellites. The possibility of momentum and energy transfer into the magnetosphere, irrespective of magnetic field line reconnection, as a specific dynamo effect, is shown. This relates statistical properties of the turbulent boundary layers with the character of the transfer through thin boundaries.

It is proposed to consider the scalings of anomalous transport (superdiffusion), determined experimentally in turbulent plasma of the Earth’s magnetosphere and laboratory plasma of thermonuclear facilities and processed using modern statistical cascade models of strong turbulence with intermittency, also within the approach of physical kinetics to the theory of plasma turbulence.

Investigation of statistical features of the magnetic fluctuations in boundary layers of Earth's magnetosphere and plasma of the solar wind, on different time scales, is carried out using magnetic field measurements from Cluster-II with a sampling frequency of 22.5 Hz in 2007-2010. We have studied the changes of shape and parameters of probability density function for magnetic fluctuations in the solar wind, foreshock region, postshock region and magnetosheath.In particular, the evolution of maximum of probability density function and the structure functions of different orders as characteristics of turbulent processes for different time scales are investigated. Structure functions of high orders are used to determine the character of turbulent processes and the resulting diffusion in these regions. We have found that the highest intermittency is observed in the postshock region. Furthermore, magnetic turbulence in the middle magnetosheath corresponds to log-Poisson turbulent cascade model, and that in the SW plasma conforms to the Iroshnikov-Kraichnan's model. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.

Statistical characteristics of plasma fluctuations in the solar wind (SW), the Earth’s magnetosphere and fusion devices are reviewed. The turbulence in all these media has a complicated multiscale structure and exhibits a generalized self-similarity in an extended scale range. The anomalous transport of mass and momentum is intermittent and is carried by sporadic plasma flux bursts with non-Gaussian statistics, long-range correlation and multifractality. Intermittent turbulent transport is characterized by superdiffusion with power law$\langle {\it\delta}x^{2}\rangle \propto {\it\tau}^{{\it\alpha}}$,${\it\alpha}\approx 1.2{-}1.8$. The structure functions in all these plasma environments are well fitted by the log-Poisson model of turbulence. Intermittent plasma turbulence displays universal properties and consists of quasi-1-D singular dissipative structures.

This chapter contains sections titled: Introduction Magnetospheric Boundary Crossings in the Cusp Vicinity on April 21, 1996 The Phenomenon Scale Studies Statistical Review Discussion and Conclusions

Three-dimensional dynamic distributions of oscillations of the magnetic field over wave vectors k have been obtained from the plasma and magnetic measurements on four satellites in the Cluster experiment in a turbulent plasma in the outer Earth’s cusp and near it. The resulting k spectra exhibit strong inhomogeneous anisotropy. The dependences of the energy of magnetic oscillations on the wavenumber have been analyzed for 288 three-dimensional spectra in the wavelength interval covering the magnetohydrodynamic and ion scales. It has been shown that the energy density of magnetic fluctuations per unit volume in the wave vector space that is averaged over the total solid angle decreases in the wavelength interval from ∼2000 to ∼10 km with an increase in according to a power law with an exponent of α = -5.0 ± 0.3 for any magnitude and character of anisotropy.

The statistical features of the magnetic field and ion flux fluctuations in the boundary regions of the Earth's magnetosphere have been studied on different timescales based on the Interball satellite measurements. Changes in the form and parameters of the probability density function have been studied for the periods when the satellite was in the solar wind plasma, different magnetosheath regions, and the turbulent boundary layer (TBL) at the polar cusp outer boundary. Variations in the probability density function maximum (P (0)) and the kurtosis value as characteristics of the turbulence property evolution on different timescales have been studied. Two asymptotic regimes of P (0), which are characterized by different power laws, have been found. The structural functions of different orders and the types of diffusion processes in different regions, depending on time variations in the generalized diffusion coefficient, have been studied in order to analyze the character of diffusion processes. For the magnetosheath regions, TBL, and polar cusp, it has been found that the diffusion coefficient increases in the course of time (i.e., the regime of superdiffusion has been obtained). In the foreshock region before the main shock, turbulent processes are described by the Kolmogorov model of classical diffusion.

A comparative analysis of the fundamental properties of fluctuations in the vicinity of boundaries in fusion plasmas and in plasmas of magnetospheric turbulent boundary layers (TBLs) shows the similarity of their basic statistical characteristics, including the scaling of the structure functions and mutifractal parameters. Important features observed include intermittent fluctuations and anomalous mass and momentum transport, due to sporadic plasma flow injections with large flow amplitudes occuring with a much higher probability than predicted for classical Gaussian diffusion. Turbulence in edge fusion plasmas and in TBLs exhibits general self-similarity in a wide range of scales extending to the dissipation scale. Experimental scalings obtained for plasma TBLs are compared with neutral fluid results, revealing the universal properties of developed turbulence. TBL scalings are described within the log-Poisson model, which takes quasi-one-dimensional dissipative structures into account. The time (tau) dependence of the mean-square displacement obtained from the experimental parameters of the log-Poisson distribution takes the form proportional to tau(alpha) with alpha approximate to 1.2-1.8 and indicates the presence of superdiffusion in the TBLs studied. Determining the nature of the generalized diffusion process from available regular data is a necessary step toward the quantitative description of TBL transport.

We study several high kinetic energy density jets observed during a traversal of the dayside magnetosheath by the Cluster spacecraft on March 17, 2001, at various distances from the magnetopause, generally characterised by anomalously high values of the local magnetosonic Mach number. We concentrate on two jets observed just outside the magnetopause, the first almost parallel to the GSM x axis and the second directed northward–tailward along the nominal magnetopause surface. We present evidence that none of them can be ascribed to magnetic reconnection at the magnetopause and show that the magnetopause is severely deformed by the jets, so that its local normal forms an angle of 97° with the quiet time magnetopause normal. On these grounds, we suggest that the indentation of the magnetopause is caused by an anti-sunward jet ramming into the magnetopause slightly equatorward of the northern cusp and that the northward–tailward jet is the result of its reflection at the deformed magnetopause. Finally, we briefly discuss our results by comparing them with past studies of events which in some way recall the one analysed herein.

We investigated the ambient plasma and magnetic field conditions at high latitudes, as well as the macroparameters of the magnetopause. For this purpose we used Cluster spacecraft plasma and magnetic field data when all the interspacecraft distances were less than 300 km. We analyzed 154 magnetosheath‐magnetosphere transitions which allow to distinguish different boundaries between the magnetosphere and the magnetosheath. First, we found transitions similar to the low‐latitude boundary layer, the plasma mantle, and cusp‐associated transitions. Second, we estimated the length of these transitions. Third, we found with high statistical evidence sub‐Alfvénic magnetosheath plasma flows just above the plasma mantle. These flows are supposed to stabilize magnetopause reconnection. Fourth, we carried out an analysis of the magnetopause pressure balance. We found a group of 24 transitions during which both the thermal and the magnetic magnetosheath pressure exceeded the magnetospheric pressure, providing conditions for unusual magnetopause formation. Fifth, for 52 magnetopause crossings we obtained the orientation as well as distributions of velocity, thickness, and current density of the magnetopause. It was found that the magnetopause with an attached plasma mantle moves slower, is thinner, and reaches higher current densities than the one with an adjacent low‐latitude‐like boundary layer. A comparison with the magnetopause at low latitudes revealed that the high‐latitude magnetopause is about two times thicker.

High-magnitude magnetic barriers in space and solar plasma are proposed to be attributed to the pile up of magnetic field lines and their Alfvénic collapse for MHD flows. The analysis of experimental data from both the Interball and Cluster spacecrafts shows that high-magnitude magnetic structures found in the Earth magnetosheath and near the magnetopause are supported by a nearly thermal transverse plasma flow, with the minimum barrier width being on the order of the ion gyroradius. The collapse termination at such scales can be explained by the balance between the pile up of magnetic field lines and backward finite-gyroradius diffusion. Comparison between the theoretical, modeling, and experimental data shows that the Alfvénic collapse is, in general, a promising mechanism for magnetic field generation and plasma separation.

On May 10, 2002 the CLUSTER spacecraft (SC) encountered a ∼450 km (five magnetosheath thermal proton gyro‐radii) wide high‐latitude magnetopause (MP). Magnetic field observations indicate the crossing of a ∼130 km thick MP current sheet (CS) located inside a magnetic hole. Proton flux measurements diagnose a dense boundary layer (BL) directly attached to the MP and an additional rare BL located earthwards from the MP. Enhanced magnetic fluctuations are found near the local proton‐cyclotron frequency Ω cp (0.4–2 Hz). Applying the phase‐differencing technique we obtained a wavelength of 150–250 km and the propagating direction earthward perpendicular to the MP. Inside the MP the pitch‐angle proton distribution demonstrates the presence of a transverse population. The formation of the two BLs can be understood by enhanced collisionless diffusion of magnetosheath protons due to wave‐particle interaction, while higher‐energy protons ( W p > 300 eV) penetrate into the BLs also via finite gyro‐radius effect.

The results of space studies are used in many applications, including the education. Work with the schools is a natural method to inform the general public about the role and value of space studies for humanity. The first RussianAustralian scientificeducational micro-satellite "Kolibri -2000" of total mass of 20,5 kg, on 20 March, 2002, has been injected into orbit of International Space Station (ISS) by separation from the transport vehicle “Progress”. It began the development of tasks for scientificeducational micro-satellite (SEM). In spite of small size, SEM had 3.6 kg of scientific payload, which provides an opportunity to carry out rather wide scientific studies both in the field of "classical" space physics and for the space weather, atmosphereionosphere connections etc., it serves also for the tasks of space education. According to the preliminary ballistic calculations, "Kolibri-2000" had to fly about 4 months; however, 17-20 April of 2002 the rapid reduction of its height began, first of all due to the increase in the Sun activity. In this paper we address the influence on the ionosphere of the processes, which occurred on the Sun of 14-24 April of 2002; changes in the flows of energetic particles, magnetic and electric fields has been examined.

The realization of Russian–Australian scientific—educational micro-satellite “Kolibri-2000” (weight of 20.5kg, http://www.kolibri2000.ru 20 March, 2002), delivered into an orbit by “Progress M1-7”, was the first item in the Program of Scientific—Educational Micro-Satellite (PSEMS' 2002–2007, http://iki.cosmos.ru/kollibri/mission1_e.htm) and designate the starting point of a series at perspective scientific—educational micro-satellites (SEMS, http://www.energia.ru/english/energia/sci-education/microsat/microsat-02.html). In the “Kolibri-2000” project, several schools equipped by School Center of Reception of the Information (SCRI), participated, including Russian schools (Obninsk http://ftschool.obninsk.org) and two Australian schools in Sydney, Knox Grammar School (www.knox.nsw.edu.au) and Ravenswood School for Girls (www.ravenswood.nsw.edu.au). The results of the “Kolibri-2000” first measurements on the orbit near the International Space Station will be submitted in this paper which include the ionosphere reaction during the April 2002 events, and address as understanding of the coupling and feedback in the Sun–Earth interaction.

The study of the interaction between collisionless plasma flow and stagnant plasma revealed the presence of an outer boundary layer at the border of a geomagnetic trap, where the super-Alfvén subsonic laminar flow changes over to the dynamic regime characterized by the formation of accelerated magnetosonic jets and decelerated Alfvén flows with characteristic relaxation times of 10–20 min. The nonlinear interaction of fluctuations in the initial flow with the waves reflected from an obstacle explains the observed flow chaotization. The Cherenkov resonance of the magnetosonic jet with the fluctuation beats between the boundary layer and the incoming flow is the possible mechanism of its formation. In the flow reference system, the incoming particles are accelerated by the electric fields at the border of boundary layer that arise self-consistently as a result of the preceding wave-particle interactions; the inertial drift of the incoming ions in a transverse electric field increasing toward the border explains quantitatively the observed ion acceleration. The magnetosonic jets may carry away downstream up to a half of the unperturbed flow momentum, and their dynamic pressure is an order of magnitude higher than the magnetic pressure at the obstacle border. The appearance of nonequilibrium jets and the boundary-layer fluctuations are synchronized by the magnetosonic oscillations of the incoming flow at frequencies of 1–2 mHz.