The Impact of Turbulence on Physics of the Geomagnetic Tail

There is a vast amount of evidence that suggests that the geomagnetic tail is like a turbulent wake behind an obstacle. Large-scale vortices in the wake are able to generate turbulent transport that takes place both along the plasma sheet, in the X and Y directions, and across the plasma sheet, in the Z direction. Thus, turbulent fluctuations in all directions should be taken into consideration when analyzing plasma transport in the plasma sheet, and stability of the plasma sheet configurations. In this review, we summarize and discuss the main results of large and middle scale magnetospheric turbulence yielded by data analysis and modeling. We also identify changes in the description of the magnetospheric dynamics connected with the existence of turbulent fluctuations in the tail.

Introduction

Formation of turbulent wake behind an obstacle is a well-known phenomenon observed in the gas and fluid flows with a high Reynolds number. An example of such a wake behind a flying bullet can be seen in Figure 1 adapted from (http://waterocket.explorer.free.fr/aerodynamics.htm). As it is well known, the sound and Alfvénic Reynolds numbers in the magnetosphere of the Earth are larger than ∼10¹¹ (Borovsky and Funsten, 2003a). The magnetic field of the Earth represents an obstacle for the solar wind flow. That is why the formation of a turbulent wake behind such obstacle is very natural even in the case of a laminar flow in front of it. In fact, the solar wind flow is not laminar, and there are many works describing its turbulent properties. On the other hand, the existence of well-defined structures and the lack of evidence of mixing in the solar wind as it moves outward through the inner heliosphere is now intensively discussed (Borovsky, 2008; Borovsky, 2020a; Borovsky, 2020b). Regardless, the main solar wind macro parameters are highly fluctuating, and the properties of the turbulent flow behind the Earth’s magnetic dipole should depend on those random fluctuations. The effect of the solar wind turbulence on the magnetospheric activity was discussed by D’Amicis et al. (2020). They show “the major role of the solar wind turbulence as a driver of geomagnetic activity especially at high latitudes” and at the same time “the geomagnetic response strongly affected by the intrinsic dynamics of the magnetosphere”. They also stressed, that “strong variations in the geomagnetic field occur even in absence of large solar wind perturbations.”

FIGURE 1

FIGURE 1. Turbulent flow behind a flying bullet (the shadowgraph).

The change of the solar wind flow at the bow shock leads to the formation of a turbulent magnetosheath behind it. The level of fluctuations in the magnetosheath is an order of magnitude larger than in the solar wind. Although the term “turbulent magnetosheath” does exist since the first space measurements (Antonova et al., 2012), the attention to the importance of the study of this phenomenon was captured mainly during the last years. Detailed reviews of such studies can be found in the current Topic Issue. The existence of turbulent magnetosheath should be taken into account during the analysis of the properties of magnetospheric turbulence and the magnetospheric dynamics.

Currently there are a lot of studies of turbulence in the Earth’s magnetosphere at the MHD scale [see, for example, references in (Borovsky et al., 2020)]. Despite this, until now the most popular analytical and computer models that describe the magnetospheric dynamics consider only the laminar flows in the geomagnetic tail. In this paper, we summarize the main results of the study of magnetospheric turbulence and try to understand the reasons of why the laminar flow models are so widely used. We also try to analyze the results of the models, which consider the turbulent transport as one of the main factors that determines the magnetospheric dynamics. A complete review of all results obtained is beyond the scope of this paper. We only try to identify the key unsolved topics in the study of the magnetospheric turbulence and to show why such studies are very important for the solution of a number of the key magnetospheric problems. Our current work is mainly concentrated on the analysis of the inertial or driving scales of tail turbulence, leaving the dissipative scale beyond the scope of this review.

The paper is organized as follows: The second section contains the historical review of the main stages of the study of the magnetospheric turbulence as well as the analysis of the properties of the turbulent transport in the geomagnetic tail. The third section contains the analysis of the main reasons, which make the studies of magnetospheric turbulent wake difficult. The fourth section is dedicated to the discussion of the results of the turbulent plasma sheet modeling. In this section, we also analyze the advantages of studies of the magnetostatic equilibrium that take into account the turbulence for the description of several magnetospheric processes. The fifth section contains the discussion of the connection between the plasma sheet turbulence and the large-scale magnetospheric convection. The six section contains the analyzes the role of the eddy diffusion in solving problems caused by the use of models based on laminar flow. The last section is dedicated to discussions and conclusions.

Study of Magnetospheric Turbulence and Its Main Characteristics

A clear manifestation of the existence of low frequency magnetospheric turbulence was obtained through spectral analysis of geomagnetic indexes [see (Consolini et al., 1996; Uritsky and Pudovkin, 1998; Stepanova et al., 2003; etc.)]. Consolini et al. (1996) examined the structure of fluctuations in the auroral electrojet index and found them to be multifractal. The noncoincidence of forms of Fourier-spectra of the solar wind parameters and the AE-fluctuation spectra shown by Uritsky and Pudovkin (1998) evidenced the existence of the inner magnetospheric sources of turbulent fluctuations of the auroral electrojets. Such finding was in close agreement with the numerous low altitude auroral observations of fluctuating electric fields, amplitudes of which are much larger than the large-scale dawn-dusk electric field. Numerous results of auroral plasma measurements also clearly demonstrated the existence of nonequipotential magnetic field lines. Turbulent fluctuations of the electric field in the plasma sheet were observed by Maynard et al. (1982), Petersen et al. (1984), Hoshino et al. (1994), etc. These fluctuations have mainly electrostatic nature.

Even the first observations in the geomagnetic tail (Sonett et al., 1960) showed the presence of strong fluctuations of the main magnetospheric parameters. It is necessary to mention that James Dungey, the author of the first theory, explaining the dependence of magnetospheric dynamics on the direction and value of the interplanetary magnetic field (IMF), considered the observed fluctuations as the main difficulty for the validity of his approach (Dungey, 1961; Dungey, 1962). He stressed the importance to study “the effect of turbulence.” However, at the beginning of the space age, the possibilities to analyze turbulent flows were limited and the systematic study of the characteristics of turbulent plasma flows have started only during the last decades.

Antonova (1985) summarized the results of magnetospheric observations leading to the suggestion about the dominant role of turbulence in the dynamics of the magnetospheric plasma sheet. It was suggested that the observed turbulence is mainly connected to the excitation of drift instabilities due to the nonhomogeneous distribution of magnetospheric plasma. It was also suggested that the magnetospheric turbulence includes embedded vortices connected to the large scale two vortex magnetospheric convection. Figure 2A shows a system of such vortices. Simultaneously Montgomery (1987) pointed out that the plasmas of the Earth's magnetotail should not behave in a laminar-flow fashion, owing to the high fluid and magnetic Reynolds numbers of the plasma sheet. He stressed that laminar-flow models of the magnetosphere and magnetotail “seem unlikely.” Unfortunately, despite of these works, most researches were convinced that it would be possible to describe the main processes in the magnetosphere in the frame of the laminar models of plasma flow.

FIGURE 2

FIGURE 2. Early schemes of the plasma sheet turbulent flows at the equatorial plane of (A)Antonova (1985), (B)Kennel (1995) and in the meridian cross section (C)Borovsky and Funsten (2003a).

The study of plasma sheet turbulence was driven by the discovery of the bursty-bulk-flow (BBF) events by Baumjohann et al. (1989), Baumjohann et al. (1990a) and the analysis of plasma sheet bulk velocity and magnetic field fluctuations (Angelopoulos et al., 1992; Angelopoulos et al., 1996; Angelopoulos et al., 1999; Borovsky et al., 1997; Borovsky et al., 1998). It was clearly shown, that the observed picture of plasma flow at the equatorial plane strongly differs from the large scale magnetospheric convection. Figure 2B shows the adapted from Kennel (1995) and discussed by Angelopoulos et al. (1999) scheme of localized bursty-flows that drive the vortical turbulent flows. It was suggested that the BBF appears as a result of reconnection processes. Not only the bulk velocity, but also the magnetic field in the plasma sheet is highly fluctuating and can result in a snarling of the magnetic field lines. Figure 2C adapted from (Borovsky and Funsten, 2003a) shows a sketch of the turbulent magnetic field of the plasma sheet constructed by adding noise to the Tsyganenko-96 magnetic field model.

The quantitative study of the hydrodynamic properties of plasma sheet turbulence started with the papers of (Borovsky et al., 1997; Borovsky et al., 1998; Borovsky and Funsten, 2003a). It was shown using the ISEE-2 plasma and magnetic field measurements that the amplitudes of the bulk velocity fluctuations are much larger than the average velocities: δVx/Vx>>1, δVy/Vy>>1 and amplitudes of the magnetic field fluctuations are comparable with its mean value δB/B ∼ 0.5. Later, Yermolaev et al. (1995) obtained the same picture in the Z and Y directions using data of the Interball/Tail probe. According to Borovsky et al. (1997), Borovsky et al. (1998), the correlation time for velocity fluctuations at geocentric distance ∼20 R_E is ∼2 min, and for the magnetic field is ∼8 min. The mixing length of the average plasma sheet is ∼10,000 km (Borovsky et al., 1998). It was shown that the distributions of the occurrence of the plasma-sheet bulk flows P (v_x) and P (v_y) has two components: i) an isotropic distribution of flows at low flow velocities and ii) an anisotropic distribution of fast flows. Such asymmetry appears due to the presence of BBF in the X and Y components of the inner plasma sheet flows. The distribution of slower flows was fitted by Borovsky et al. (1997) by the exponential functions:$P\left(V_x\right)=0.32\exp \left(-\left|V_{x-8}\right|/41\right)$, $P\left(V_y\right)=0.31\exp \left(-\left|V_{y-5}\right|/54\right)$, where Vx and Vy are the velocities in X and Y directions, and the velocities have units of km⋅s⁻¹, reaching a very high correlation with the correlation coefficients equal to 0.98. The distribution of fast BBF flows was fitted by $P\left(V_x\right)=0.300\exp \left(-\left|V_X\right|/149\right)$ for V_x > 0 and $P\left(V_x\right)=0.011\exp \left(-\left|V_x\right|/159\right)$ for V_x < 0. The analysis of the properties of velocity fluctuations made it possible to conclude [see (Angelopoulos et al., 1999)] that the geomagnetic tail is a system that exhibits sporadic variability and has properties of intermittent turbulence. This conclusion was supported by the subsequent studies showing that magnetic fluctuations in the near-Earth magnetosphere exhibit multiscale features (Lui, 2001; Consolini et al., 2005).

Borovsky et al. (1997) and Borovsky and Funsten (2003a) showed that the plasma-sheet material appears to be well mixed in density and temperature. They stressed that the persistent (many-minute) laminar flow is not observed and the turbulence may be strongly driven rather than well developed. It is interesting to mention that the values of plasma flow are significantly larger during the intervals of steady magnetospheric convection than they are during active times. Neagu et al. (2002), Neagu et al. (2005) found no significant dependence of the amplitude of the ion velocity and magnetic field fluctuations on the distance from the Earth toward the geomagnetic tail, the dawn-tail distance and on the distance from the neutral sheet.

Subsequent results obtained by Antonova (2000), Ovchinnikov et al. (2000), Schödel et al. (2001), Ovchinnikov et al. (2002), Troshichev et al. (2002), Uritsky et al. (2002), Neagu et al. (2002), Uritsky et al. (2003), Neagu et al. (2005), Stepanova et al. (2005), Stepanova et al. (2006), Antonova (2008), Uritsky et al. (2008), Stepanova et al. (2009), Uritsky et al. (2009), Stepanova et al. (2011), etc. supported the validity of early findings and permitted to obtain a number of statistical dependencies. Ovchinnikov et al. (2002), Stepanova et al. (2005), Stepanova et al. (2009), Stepanova et al. (2011) showed that the level of velocity fluctuations strongly depends on the phase of magnetospheric substorm. It increases after a substorm onset and then slowly decreases during 1–2 h.

The BBFs are frequently considered as the main source of the observed plasma sheet fluctuations. They are composed by flow bursts lasting ∼1 min and are commonly observed at substorm growth, expansion and recovery phases. Nonetheless, many BBF occur without classical substorm signatures during pseudo-breakups and auroral brightening. The BBF occurrence rate peaks close to midnight, and the variance of the remnant flow during high AE is stronger at midnight than at nearby sectors. This result supports the conclusion of Kennel (1995) that the geomagnetic tail is in a state of bimodal convection, whereby the potential flow is stagnant unless it is driven by localized flow bursts. Nagai et al. (1998) showed using the Geotail observations that the fast flows tend to be observed around the near-Earth pre-midnight sector. Petrukovich et al. (2001) calculated the angles between the vectors of fast earthward plasma flow and the local magnetic field. In the low-β (where β is the plasma parameter) parts of the geomagnetic tail, the fast flows were found to be nearly field-aligned. In the high-β plasma sheet the average angle was larger than 45°. The width of the flow channel, which represents the typical large-scale characteristic scale of the flow used to calculate the Reynolds number, has been estimated from the statistical analysis of Cluster spacecraft multi-point measurements by Sergeev et al. (2000), Nakamura et al. (2004). It was shown that the full width of the flow channel is 2–3 R_E in the “dawn-dusk” direction and 1.5–2 R_E in the “north-south” direction. Recently Sitnov et al. (2019) summarized the main results of the BBF study.

Borovsky et al. (1997) found that within the plasma sheet the slope of the power spectral density vs. frequency for plasma flow velocity and magnetic field varied from −0.8 to −2.0 and from −1.6 to −3.0, respectively. Different types of Reynolds numbers can be derived for the flows in the plasma sheet reflecting different aspects of turbulent flows (Borovsky and Funsten 2003a; Weygand et al., 2005). In particular, Weygand et al., (2005) showed that the level of intermittency in the central plasma sheet differs from that observed for the outer plasma sheet. They examined the magnetic field spectral indices in the field-aligned coordinate system and found that their range was quite broad (average of −2.0 ± 0.4). The transverse magnetic field component inside the central plasma sheet in the Y direction had a spectra index of −1.56 ± 0.04, and the mean eddy scale size found in this study was 6,000 km.

The study of plasma velocity fluctuations has been limited by a low time resolution of particle spectra measurements in comparison to the magnetic measurements, and by contamination caused by many sources. That is why the main progress in the study of plasma sheet turbulence was done due to the analysis of spectra of magnetic fluctuations using Cluster magnetometer observations (Vörös et al., 2003; Vörös et al., 2004; Vörös et al., 2006; Vörös et al., 2019; Volwerk et al., 2004; Weygand et al., 2005). It was shown, that the turbulence in the plasma sheet is a mixture of Alfvénic wavy turbulence and of eddy 2-D turbulence. A strong correlation between the maximum perpendicular flow velocity and the turbulence power for maximum velocities 150 ≤ v_⊥max≤ 400 km/s was found. It was also shown that the presence of BBFs significantly changes the spectral index or scaling index. Hoshino et al. (1994) showed that fluctuations of the magnetic field observed in the distant plasma sheet are characterized by a “kink” Fourier power law spectrum that can be approximated by two power law functions with two different spectral indices (Zelenyi et al., 2015).

The behavior of magnetospheric turbulence is hard to comprehend because it is almost impossible to discriminate between spatial and temporal variations even using data from multipoint satellite missions as THEMIS, CLUSTER and MMS. That is why the determination of properties of magnetospheric turbulence in most cases is still limited to the method proposed by Borovsky et al. (1997), Borovsky et al. (1998) for calculations of fluctuations of hydrodynamic velocities and their autocorrelation times [see also (Ovchinnikov et al. (2000), Antonova (2000), Ovchinnikov et al. (2002), Antonova (2008); Troshichev et al. (2002)] for the implementation of this method). It allows us to determine the turbulent flow velocities v_rms and their components and the autocorrelation time τ_auto when the mean flow velocity is small compared with the turbulent flow velocities. Borovsky et al. (1997) considered the autocorrelation time as a measure of the persistence of a fluctuating velocity and calculated it by analyzing the autocorrelation function:

$A\left(\tau \right)=\frac{\text{Σ}\left(V_{rms}\left(t\right)-V_{rms}\left(t\right)\right)\left(V_{rms}\left(t+\tau \right)-V_{rms}\left(t+\tau \right)\right)}{{\left(V_{rms}\left(t\right)-V_{rms}\left(t\right)\right)}^2}(1)$

Four methods were proposed for the determination of τ_auto (Borovsky et al., 1997), the most popular of which is based on the determination of the time interval during which the curve A (τ) has fallen to the value A (τ) = 1/e. Finally, the method proposed by Borovsky et al. (1998) permits to estimate the coefficient of eddy diffusion as:

$D={\left(V_{rms}\right)}^2{\tau }_{auto}/2(2)$

and analyze the transport of the plasma sheet material.

The first evaluation of the coefficient of eddy diffusion made by Borovsky et al. (1998) gave a very high value of D = 2.6∙10⁵ km² s⁻¹. Nearly the same eddy diffusion coefficients were reported by (Ovchinnikov et al., 2000; Stepanova et al., 2005; 2009; Stepanova et al., 2011; Pinto et al., 2011). In particular, Stepanova et al. (2009), Stepanova et al. (2011) obtained the statistical distribution of the coefficients of eddy diffusion for quiet time and different phases of magnetospheric substorm. The use of the Interball/Tail probe satellite data allowed Stepanova et al. (2009) to determine D_zz and D_yy components of the eddy diffusion tensor, meanwhile the use of the THEMIS satellites permitted to obtain all three diagonal components of this tensor D_zz, D_yy and D_xx (Stepanova et al., 2011). However, it is necessary to mention that the presence of BBF might strongly affect the results of D_xx calculations and this value should be used with caution. Figure 3A shows the comparison of the dependence of D_zz on the radial distance for different phases of the magnetospheric substorm from (Stepanova et al., 2009) (red diamonds) and (Stepanova et al., 2011) (green diamonds). Figure 3B shows the same results for D_yy from (Stepanova et al., 2009) (blue squares) and (Stepanova et al., 2011) (dark blue squares). It is possible to note that the eddy diffusion coefficients obtained using the data from the THEMIS mission are smaller than the coefficients obtained from the Interball/Tail probe observations. It can be explained considering that during the first years of the THEMIS mission the geomagnetic activity was very low, and the eddy diffusion is expected to be lower for the time interval used for that studies (2008–2010). Pinto et al. (2011) obtained the instantaneous radial distribution of eddy diffusion coefficients using the data of the THEMIS satellites located along the midnight meridian. It was shown that the level of turbulence is greatly decreased at geocentric distances smaller than ∼10 R_E. Slightly lower values of eddy diffusion coefficients were obtained in the distant tail by Troshichev et al. (2002). The same eddy diffusion coefficient values ∼10⁵ km²/s were obtained by Nagata et al. (2008) for northward IMF orientation. Wang et al. (2010) analyzed plasma sheet transport and estimated the diffusion coefficients D_yy and D_xx associated with fluctuating drift to be ∼10⁵–10⁶ km²/s.

FIGURE 3

FIGURE 3. Comparison of the dependencies of D_zz(A) and D_yy(B) on the radial distance and on the phase of magnetospheric substorm (q, quiet; exp, expansion; rec, recovery) from (Stepanova et al., 2009) (red diamonds and blue squares) and (Stepanova et al., 2011) (green diamonds and dark blue squares).

As it will be shown in the next sections, the introduction of eddy diffusion transport makes it possible to overcome the limitations of the ordinary MHD approach for the description of large-scale magnetospheric processes. To date, the necessary formalism has been developed only for gases in the absence of a magnetic field (Klimontovich, 1990; Klimontovich, 1999). Nonetheless, even a simplified analysis could be very useful.

Reasons for the Popularity of Laminar Flow Models

Our analysis of characteristics of turbulent plasma flows leads to a natural question: Why do the most popular models describe the magnetospheric plasma flows in a laminar fashion? They have been developed in parallel with the models of the radiation belts formation, where the radial diffusion is recognized as the most important mechanism. The simplest answer is because of the real simplicity of such models and the possibility in a number of cases to obtain more or less reasonable results. Nonetheless, the explanation of this popularity is not so simple and can be related to three main reasons.

The first reason is a comparatively small number of works dedicated to the magnetospheric turbulence in comparison with the solar wind turbulence. It is related to the viability of use of the Taylor’s hypothesis for the solar wind, which allows us to transform the length scale l into the time scale t via a simple relation: l = t × V_SW, where V_SW is the solar wind velocity. This relation permits in case of the solar wind to obtain spectra of turbulent fluctuations in a wide range of scales, meanwhile it is very difficult or even impossible to separate spatial and temporal variations inside the magnetosphere, especially for large vortices, even using multisatellite observation.

The second reason is that the plasma sheet configuration differs from the turbulent wake in hydrodynamic fluid. The scale of plasma sheet in Z direction is much smaller than the scale in Y direction. The formation of the plasma sheet is possible to model using global MHD codes and assuming the preexistence of particle sources in the magnetosphere [see (Watanabe and Sato, 1990) and results of later MHD simulations]. As a result of this modeling, the plasma sheet region extends widely in the equatorial plane and is considerably compressed perpendicular to it. However, taking into account the high values of the coefficient of eddy diffusion D_zz it is difficult to understand why such configuration could exist for a comparatively long time. In the next section we shall show that the observed structure of the quasistable magnetospheric turbulent wake as a sheet-like structure can be clearly explained taking into account the compression of this wake by the dawn-dusk electric field.

The third, and from our point of view the most important reason is related to the problem of the auroral oval mapping. Even the first results of auroral observations (Chamberlain, 1961) showed that the quiet time auroral arcs could exist for many hours, which is difficult to imagine if the roots of such arcs are embedded into the turbulent medium. For a long time, it has been widely assumed that the auroral oval maps to the plasma sheet. This assumption was based on the use of the magnetic field models with predefined configuration of current systems (Antonova et al., 2018). Nonetheless, the results of the topological mapping, based on the use of the plasma pressure as a “tracer” along a magnetic field line, indicated (Antonova et al., 2014; Antonova et al., 2015), that most of auroral oval is mapped to the surrounding the Earth plasma ring at geocentric distances from ∼7 to ∼10 R_E (Kirpichev et al., 2016). As the level of velocity and magnetic field fluctuations decreases at the distances <10 R_E (Stepanova et al., 2009; Stepanova et al., 2011; Pinto et al., 2011), the roots of quiet auroral arcs can be formed in a comparatively stable region. Therefore, the third obstacle to model the magnetosphere as a turbulent wake is caused by an erroneous auroral oval mapping.

Turbulent Plasma Sheet Modeling

The experimental evidences of high levels of fluctuations having a turbulent character encourage the development of models that would take into account both the turbulent transport and the modification of particle distribution functions due to interaction with turbulent electric and magnetic fields. It is an endeavor that could be reached in the future. For now, we can only present a few results, which can be useful for the future studies.

MHD Models and Plasma Sheet Turbulence

The most popular models of the large scale magnetospheric dynamics, known as the ideal MHD models, are developed using the MHD finite difference codes. That is why the results of such modeling should be used with caution taking into account the effect of numerical resistivity. Frequently such numerical codes break the frozen-in condition and are not able to produce high magnetic Reynolds numbers. These models reproduce the magnetic field line reconnection in the geomagnetic tail at different distances depending on the grid spacing scale. Nonetheless, even this kind of models reproduce the formation of medium scale vortexes in the plasma sheet after reconnection (Birn et al., 1999; Birn et al., 2011). It is necessary to mention also that MHD models describe the formation of vortices that appeared due to development of Kelvin-Helmholtz instability at the magnetospheric flanks stating from (Miura, 1984). Latest results employed the fully kinetic model were obtained by (Nakamura et al., 2020).

When the computer codes combine both the low resistivity and small grid spacing, it is possible to obtain comparatively large values of the magnetic Reynolds number and to model the formation of the turbulent plasma sheet under idealized southward (El-Alaoui et al., 2010) and northward (El-Alaoui et al., 2012) IMF. These models were able to reproduce some features of the plasma sheet turbulence, including the nested vortices at multiple scales. The largest scales were associated with the reconnection outflows and the diversion of high-speed flows. El-Alaoui et al. (2010), El-Alaoui et al. (2012) also found that the power spectral densities (PSDs) had the characteristics of a turbulent flow and showed the three scale ranges expected from theory: the energy-containing range, the inertial range, and the dissipative range. They selected the formation of localized reconnection regions as the main process driving turbulence in the plasma sheet.

However, the appearance of numerical resistivity is not the unique and even not the main problem of the ideal MHD models. It is necessary to take into account that the contribution of the pressure gradients in the generalized Ohm’s law can be significant. In collisionless plasma, this law has the form:

$\mathbf{E}+\left[\mathbf{V}\times \mathbf{B}\right]=\frac{\left[\mathbf{j}\times \mathbf{B}\right]}{\mathit{ne}}-\frac{\nabla {\mathit{p}}_{\mathit{e}}}{\mathit{ne}}+\left[\frac{\partial \mathbf{j}}{\partial \mathit{t}}+\nabla \cdot (\mathbf{j}\mathbf{V}+\mathbf{V}\mathbf{j})\right]\frac{{\mathit{m}}_{\mathit{e}}}{\mathit{n}{\mathit{e}}^2}(3)$

where m_e and n_e are the mass and density of electrons, m_i and n_i are the mass and density of ions, $\mathit{m=}{\mathit{m}}_{\mathit{i}}\mathit{+}{\mathit{m}}_{\mathit{e}}\mathit{,n=}\left({\mathit{m}}_{\mathit{i}}{\mathit{n}}_{\mathit{i}}\mathit{+}{\mathit{m}}_{\mathit{e}}{\mathit{n}}_{\mathit{e}}\right)/\mathit{m}$ is the density, $\mathit{V=}\raisebox{1ex}{$\left({\mathit{m}}_{\mathit{i}}{\mathit{n}}_{\mathit{i}}{\mathit{v}}_{\mathit{i}}\right)\mathit{+}\left({\mathit{m}}_{\mathit{e}}{\mathit{n}}_{\mathit{e}}{\mathit{v}}_{\mathit{e}}\right)$}\!\left/ \!\raisebox{-1ex}{$\mathit{mn}$}\right.$ is the plasma velocity, j = en (v₋v_e) is the current density, E is the electric field. The frozen-in approximation can be used only in the regions where the right-hand side of the generalized Ohm’s law is much smaller than its left-hand side (Baumjohan and Treuman, 1996; Priest and Forbes, 2000; Paschmann et al., 2002; etc.). It is necessary to mention that the ideal MHD do not consider the electrostatic field and the induction equation can be written as (Priest and Forbes, 2000):

$\frac{\partial \mathbf{B}}{\partial \mathit{t}}=\nabla \times \left(\left[\mathbf{V}\times \mathbf{B}\right]-\frac{1}{\mathit{ne}}\left[\mathbf{j}\times \mathbf{B}\right]-\frac{\nabla {\mathit{p}}_{\mathit{e}}}{\mathit{ne}}-\frac{{\mathit{m}}_{\mathit{e}}}{\mathit{n}{\mathit{e}}^2}\frac{\partial \mathbf{j}}{\partial \mathit{t}}\right)(4)$

The first term in the right-hand side of Eq. 3 is named the Hall term. Priest and Forbes (2000) stressed that only in case of strong collisional plasma in weak magnetic field this term can be neglected. The scale of the Hall term if V ≠ V_A is equal (Priest and Forbes, 2000):

${\mathit{L}}_{\mathit{Hall}}={\mathit{\lambda }}_{\mathit{i}}\frac{{\mathit{V}}_{\mathit{A}}}{\mathit{V}}(5)$

where ${\mathit{\lambda }}_{\mathit{i}}\mathit{=}\mathit{c}/{\mathit{\omega }}_{\mathit{pi}}$ is the ion inertial length, ${\mathit{\omega }}_{\mathit{pi}}\mathit{=}{\left[\left({\mathit{e}}^{\mathit{2}}\mathit{ne}\right)/\left({\mathit{\epsilon }}_{\mathit{0}}{\mathit{m}}_{\mathit{i}}\right)\right]}^{\raisebox{1ex}{$\mathit{1}$}\!\left/ \!\raisebox{-1ex}{$\mathit{2}$}\right.}$ is the ion plasma frequency, c is the velocity of light, ε₀ is the vacuum dielectric constant. Therefore, in the regions of slow flow velocity where V_A>> V, the ideal MHD becomes inapplicable and the Hall MHD must be used. The ideal MHD models are used in thermonuclear researches for the description of the aperiodic instabilities and the study of quick processes. The slow plasma processes can be described using the Hall MHD, which requires large computer capacities. However, it is clear that inside regions of turbulent flow in the plasma sheet only regions with near to Alfvénic plasma flow can be analyzed properly using the ideal MHD approach. Eqs. 3, 4 contain also the term, which depends on the electron pressure gradient. This leads to the validity of the frozen in conditions for the electron motion by neglecting the electron inertia term (Baumjohan and Treuman, 1996):

$\frac{\partial \mathbf{B}}{\partial \mathbf{t}}=\nabla \times \left[{\mathbf{v}}_{\mathbf{e}}\times \mathbf{B}\right](6)$

This means that in collisionless MHD with Hall currents, the electrons are the unique plasma component, which is frozen to the magnetic field. The plasma flow in such a case deviates from the motion of the magnetic field lines. Hall currents are observed in the magnetotail [see Nagai et al. (2003) and later observations]. The validation of the frozen in condition for electrons and electron reconnection was one of the main goals of the MMS mission (Burch et al., 2016a). The electron reconnection was used to explain the observations of the super-Alfvénic electron jets, not accompanied by the ion outflows (Burch et al., 2016b; Phan et al., 2018). Although the MMS observations captivated the attention to the study and modeling of the turbulent processes at small and medium scales [see (Stawarz et al., 2015; Ergun et al., 2018; Califano et al., 2020) and references therein], it is not clear how these studies could help to clarify the main properties of the large-scale magnetospheric dynamics.

Therefore, in spite of significant advantages of different MHD models in the analysis of magnetospheric turbulence and dynamics, there are some important problems which solution requires a different approach. This includes the magnetospheric configurations with slow in comparison with the Alfvén velocity plasma motions like the central plasma sheet where the averaged flow velocities are ∼30 km/s (Angelopoulos et al., 1993), and hence V << V_A. At the same time, for this and similar regions it is necessary to take into account the presence of the turbulent eddy diffusion and the role of the turbulent transport due to the large values of obtained eddy diffusion coefficients.

It is well known that when the flow velocity is much smaller than the Alfvén and sound velocities, the analyzed plasma configuration is in magnetostatic equilibrium [j × B] = ∇p. Here we discuss the simplest case of the isotropic plasma pressure. Plasma velocity across the plasma sheet is fast only in case of the tail flapping; meanwhile plasma velocity along the sheet is comparable with the Alfvén velocity only inside the BBF. Therefore, it is possible to analyze the properties of the plasma sheet using the condition of magnetostatic equilibrium as it was done in many papers. It is necessary to note that the existence of stress balance p + (B²/2μ₀)≈const across the plasma sheet and the plasma pressure isotropy were experimentally verified by Baumjohann et al. (1990b), Kistler et al. (1993), Petrukovich et al. (1999), Wang et al. (2013), etc. The plasma sheet is a well-defined structure that exists in spite of the presence of turbulent fluctuations. Therefore, it is necessary to understand why such structure is formed and how it is supported in the collisionless plasma with turbulent fluctuations. It is necessary to mention that the existence of high level of turbulent fluctuations can lead to the appearance of eddy viscosity (Borovsky and Funsten, 2003b). Nonetheless, the eddy diffusion transport is more relevant for the Earth’s plasma sheet where plasma pressure is nearly isotropic.

Model of the Turbulent Plasma Sheet Including Eddy Diffusion and Pressure Balance Across the Plasma Sheet

In order to include the turbulent transport to the description of the large-scale processes in the geomagnetic tail it is necessary to use a special system of hydrodynamic transport equations. To our knowledge, such system of equations has not been developed for collisionless plasma yet. However, the turbulent diffusion was included to the system of hydrodynamic equations by Klimontovich (1990), starting from the equation of mass conservation, which can be written as:

$\frac{\partial \mathit{\rho }}{\partial \mathit{t}}+\frac{\partial }{\partial \mathbf{r}}\left(\mathit{\rho }\mathbf{V}-\mathit{D}\frac{\partial \mathit{\rho }}{\partial \mathbf{r}}\right)=0(7)$

where ρ is the mass density, V is the bulk velocity (averaged on turbulent fluctuations) and D is the space diffusion coefficient. In a presence of the magnetic field, the coefficients of space diffusion can have different values along and perpendicular to the magnetic field and are determined by the properties of the turbulence. Taking into account such feature, Eq. 7 can be used in the first approximation for the description of plasma transport. It shows that the distribution of plasma density does not change if the expression in round brackets is equal to zero, leading to the appearance of quasistatic distributions.

Observed conservation of pressure balance across the plasma sheet permits to use the condition of magnetostatic equilibrium as an empirical relation thereby connecting the magnetic field and the plasma pressure. A more careful analysis will require the inclusion of magnetic field fluctuations. However, at first approximation it is possible to suggest that they are not so large in comparison with the regular field [∼0.5 in accordance with (Borovsky et al., 1997)]. In this case, it is possible to solve the Grad-Shafranov equation and to determine the magnetic field distribution across the plasma sheet in the tail approximation of Birn and Schindler (1983).

Such approach was used in the Antonova and Ovchinnikov (1996a; Antonova and Ovchinnikov,1996b; Antonova and Ovchinnikov, 1999; Antonova and Ovchinnikov, 2001) model developed to explain the existence of the quasistable plasma sheet in the presence of turbulent transport. As it was mentioned in Reasons for the Popularity of Laminar Flow Models, the concept of the plasma sheet as a turbulent wake behind an obstacle has attracted little attention due to an unusual configuration of such turbulent wake, in comparison to the wake commonly observed in ordinary fluids. In the geomagnetic tail, it only takes up part of the volume behind the obstacle and is located between the tail lobes. However, it is well known that such configuration is observed only under southward IMF orientation (IMF Bz < 0). When the IMF turns northward for a comparatively long time, the tail lobes fill with plasma from the plasma sheet (Frank et al., 1986). Such filling leads to the appearance of polar cap arcs and the formation of theta-aurora. One of the main differences between the periods of IMF Bz < 0 and of IMF Bz > 0 is the value of the dawn-dusk electric field, which is much stronger for the southward IMF orientation. The particle drift along the Z axis in the SM coordinate system generates the lobe plasma flow directed from the tail lobes to the center of the plasma sheet, where the plasma density has a maximum. Eq. 5 shows that the turbulent transport, directed opposite to the plasma pressure gradient, can compensate the regular transport if the averaged bulk velocity $V_z{D}_{zz}{\rho }^{-}d\rho /dz$. Due to the intense plasma mixing, the plasma temperature variations across the plasma sheet are much smaller than the variations of the plasma density. Therefore, the plasma density can be obtained from the condition of the pressure balance across the plasma sheet, considering that the temperature is constant. The regular velocity V_z can be evaluated using, for example, the models of the dawn-dusk electric field. By equating regular and turbulent transports, it is possible to obtain the value D_zz necessary for the existence of the plasma sheet between the tail lobes, as shown schematically in Figure 4.

FIGURE 4

FIGURE 4. Scheme illustrating the formation of the turbulent plasma sheet. Case (A) corresponds to the expansion of the sheet due to eddy diffusion when the regular flow velocity V = 0, case (B) corresponds to the quasistable configuration, when the regular velocity to the tail center compensates the eddy diffusion.

Figure 5 shows an example of plasma pressure distribution obtained using (Antonova and Ovchinnikov, 1996a; Antonova and Ovchinnikov,1996b; Antonova and Ovchinnikov, 1999) model at geocentric distances X = −30 R_E when $B_z^{IMF}<-4nT$ (a), and at $B_z^{IMF}>+4nT$ (b). The values of the dawn-dusk electric field were obtained from the Volland-Stern electrostatic field model at ionospheric altitudes, and subsequent mapping to the tail using the Tsyhanenko-87W magnetic field model. The ratio of plasma pressure values between neighboring contours is e^1/2. This model explains the thinning of the plasma sheet during the substorm growth phase due to the increase of the dawn-dusk electric field. It also explains the plasma sheet thickening after substorm onset due to the increase of the level of turbulence and the eddy diffusion. The filling of the tail lobes during IMF Bz > 0 was explained due to strong reduction of the dawn-dusk electric field under the northward IMF orientation.

FIGURE 5

FIGURE 5. An example of plasma pressure distribution in the plasma sheet at geocentric distance X = −30 R_E, (A) when $B_z^{IMF}<-4nT$ and (B) at $B_z^{IMF}>+4nT$, in accordance with the model of Antonova and Ovchinnikov (1999).

The main achievement of the discussed model is the prediction of the value of the eddy diffusion coefficient D_zz by Antonova and Ovchinnikov (1996a), Antonova and Ovchinnikov (1996b), before it was obtained experimentally in many works, starting from Borovsky et al. (1998) [see the discussion in (Antonova, 2000; Ovchinnikov et al., 2000; Ovchinnikov and Antonova, 2017)]. Later, Stepanova and Antonova (2011) made a direct verification of the main predictions of the model. Despite its simplicity, the discussed model shows how the existence of turbulent transport could explain the observed formation of quasistable structures, which are compressed by the regular plasma motions, compared with the classical schemes where such compression leads to the appearance of reconnection.

Large Scale Magnetospheric Vortices and Magnetospheric Turbulence

To date the mechanisms of the formation of the plasma sheet turbulence are not clear, and continue to be discussed. The formation of the large-scale vortices with scales ∼10,000 km is of particular interest, as they make the main contribution to the turbulent transport. The existence of magnetospheric vortices was first demonstrated using data of simultaneous ISSE-1 and ISEE-2 observations by Hones et al. (1979) and analyzed in detail by Birn et al. (1985). Study and modeling of such vortices were later connected to the development of Kelvin-Helmholtz instability at the magnetospheric flanks. Latest analysis of Nakamura et al. (2020) showed how the formation of vortices is related to the level of solar wind fluctuations.

Study of BBF formation leads to the description of vortex formation at the center of the plasma sheet. According to the model of Birn et al. (1999), Birn et al. (2011), the vortices could appear as a result of reconnection. The large-scale vortices of such type were successfully identified in many works using multisatellite observations (Keiling, et al., 2009; Keika et al., 2009; Panov et al., 2010; Tang, 2012; etc.). Unfortunately, these studies were done in (X, Y) plane only, and the structure of vortices in Z direction remains unclear.

El-Alaoui et al. (2010), El-Alaoui et al. (2012) considered the energy-containing scale of magnetospheric turbulence as the largest scale being associated with reconnection outflows and the diversion of high-speed flows. Therefore, the eddy vortices were considered as a driving or integral scale of the tail turbulence. Nonetheless, the appearance of such vortices is a consequence of the large-scale magnetospheric flows. These flows increase when IMF Bz < 0. That shows their deep connection with the large-scale magnetospheric convection. A strong connection between the eddy diffusion and the large-scale magnetospheric convection is also described in the model of the turbulent plasma sheet proposed by Antonova and Ovchinnikov (1996a), bAntonova and Ovchinnikov (1996b), Antonova and Ovchinnikov (1999).

Properties of the large-scale magnetospheric convection have been obtained by many tools and are well known [see (Weimer, 1996)]. The nature of the observed large-scale magnetospheric convection was widely discussed in multiple works since the beginning of Space Age. The viscous interaction and reconnection models were the most popular ones for a long time. However, both mechanisms were not considered a source of large-scale vortices at driving or integral scale of turbulence. Borovsky et al. (2020) stressed that the viscous interaction is neither quantified nor understood. The observed high level of magnetosheath and plasma sheet turbulence is the main obstacle to the applicability of the Dungey (1961) reconnection model.

The discovery of a system of large-scale field-aligned currents by Iijima and Potemra (1976) was crucial for the understanding of the large-scale magnetospheric convection. It became clear that the dawn-dusk electric field in the polar cap and, hence, the large-scale two vortex magnetospheric convection are supported by the Region I field-aligned currents of Iijima and Potemra. The source of the Region 1 currents in the equatorial plane is located inside the plasma sheet and the outer part of the ring current (Antonova et al., 2006; Xing et al., 2009; Antonova et al., 2018). The most probable mechanism of generation of both Region II and Region I currents is related to the existence of the plasma pressure gradients. Strong arguments in favor this mechanism were provided by Troshichev (1982). In particular, Antonova and Ganushkina (1997) showed that the Region I field-aligned currents can be supported by the azimuthal plasma pressure gradients, which appear due to azimuthal asymmetry of the magnetoshere modulated by the IMF. The detailed discussion about the action of this mechanism is beyond the scope of this paper. For the description of turbulent processes in the magnetosphere, it is only important to stress that such mechanism produces the large-scale two vortex convection flows.

The inverted V structures in the auroral oval containing the field-aligned potential drop are a clear result of a medium scale vortex formation in the region of the upward field-aligned current (see Figure 1 in (Antonova and Ovchinnikov, 1999) which schematically shows the structure of the electrostatic field and its equipotentials typically observed in the inverted-V quiet auroral band). It is necessary to remind that the electric field in the inverted V structure is much larger than the large-scale dawn-dusk electric field, and it increases with the distance from the ionosphere. We assume that the medium-scale vortices such as inverted-V structures should form part of the plasma sheet turbulence. However, their connection with smaller vortices that produce the eddy diffusion in the plasma sheet is not clear yet.

Our analysis shows that mechanisms of generation of the plasma sheet turbulence are deeply connected to the plasma pressure gradients in the magnetosphere, including the driving or integral scale vortices–the two-vortex convection and the eddy vortices, responsible for the eddy diffusion transport.

How the Incorporation of the Eddy Diffusion Helps to Solve Problems Caused by the Use of Models Based on Laminar Flow

The convection crisis is one of the main problems of the slow motion of plasma from the tail to the Earth inside the plasma sheet. Ericson and Wolf (1980), Birn and Schindler (1983) showed that the adiabatic plasma transport in case of the laminar convection should lead to an increase of plasma pressure in the plasma sheet, which was never observed. The adiabatic laminar convection assumes the conservation of particles in a magnetic flux tube and an increase of their temperature in accordance with the adiabatic law, i.e. particle and heat fluxes between the flux tubes are not allowed. Analyzing this problem, Kivelson and Spence (1988) showed that under quiet geomagnetic conditions a quasi-static adiabatic convection is possible in a magnetotail of finite width. However, the problem continued to exist for more disturbed conditions. The existence of turbulent electric field fluctuations and eddy diffusion naturally removes this problem (Antonova, 1985; Antonova and Tverskoy, 1998), as the turbulent fluctuations of the magnetic field do not allow to use such concepts as the magnetic flux tube and the adiabatic transport. It is necessary to note also that particle trajectory in fluctuating magnetic and therefore fluctuating electric field becomes stochastic, when the Larmor radius of a particle is comparable with the field inhomogeneity. In contrast to the commonly used adiabatic model, the behavior of particle pressure in the plasma sheet was determined by Antonova and Ovchinnikov (1996a), Antonova and Ovchinnikov (1996b), Antonova and Ovchinnikov (1999) as the pressure balance in Z direction described by the flaring-tail model of Tverskoy (1968) and Kennel (1995).

Consideration of the high level of plasma sheet fluctuations is also fundamental for the understanding of the nature of magnetospheric substorms. According to (Akasofu, 1964), an isolated substorm onset starts with the brightening of the equatorward auroral arc. Such arc is mapped to the equatorial plane at geocentric distance ∼7 R_E [see arguments summarized by Antonova et al. (2018)], i.e., near the inner boundary of the outer part of the ring current. Dispersionless injection boundary is also located at such distances (Lopez et al., 1990; Spanswick et al., 2010). Such features mean the development of an instability able to produce auroral brightening and local particle acceleration. It is difficult to imagine how this instability would develop in the presence of turbulent fluctuations in the plasma sheet, assuming that the auroral oval is mapped to that region, as suggested in many works. On the contrary, the mapping of the auroral oval to the outer part of the ring current does not lead to such consequences, considering that the level of turbulent fluctuations before substorm vanishes in this region, as mentioned in Study of Magnetospheric Turbulence and Its Main Characteristics.

It is necessary to mention, that the BBFs are frequently discussed as an onset trigger in the tail. They are observed during the substorm growth, expansion and recovery phases. Nonetheless, many BBFs occur without classical substorm signatures during pseudo-breakups and auroral brightening and produce the auroral streamers. Many substorm onsets are not preceded by the arrival of streamers [see references in (Antonova et al., 2009; Sitnov et al., 2019)]. Therefore, the existence of plasma sheet turbulence including BBFs is a strong argument in favor of the location of the instability responsible for a substorm onset at comparatively small geocentric distances, that agrees with the onset observations.

During a long history of study of substorms different mechanisms of substorm onset were discussed. Most models based on the reconnection in the tail suppose the existence of the laminar plasma flow and the regular character of the magnetic field before the reconnection onset including the models which take into account the Hall term and electron inertia [see, for example (Shay et al., 2003)]. Therefore, variations of plasma sheet velocity and magnetic field constantly observed in the plasma sheet create real difficulties for such models, giving preference for models of substorm onset located at geocentric distances <10 R_E such as the current disruption models (Lui, 2001) and development of upward field-aligned current instability (Antonova, 2002; Stepanova et al., 2002).

One more problem, which naturally appears in connection with the plasma sheet turbulence, is the presence of beams and fast plasma motions, which are attributed to the magnetic reconnection leading to the change of a large-scale magnetic configuration. However, as was mentioned earlier, most of the BBFs do not produce any substantial changes like generation of geomagnetic substorms. To understand such contradiction, it is necessary to remind that the plasma sheet turbulence is a mixture of the Alfvénic wavy turbulence and eddy 2-D turbulence. Therefore, the Alfvénic disturbances constantly exist in the plasma sheet. Relations (3) and (4) show that the ideal MHD in such a case is applicable when the scale of perturbed region is larger than the ion inertial length. This means that the traditional reconnection models can describe the processes inside such regions, which can be only a small part of the entire turbulent region. In such a case, the local reconnection phenomena can be considered as an intrinsic property of the collisionless turbulence and local reconnection phenomena leading to the BBF formation as a part of the tail turbulence development. The reconnection-like phenomena observed inside the turbulent magnetosheath (Yordanova et al., 2016; Vörös et al., 2017) and the plasma sheet (El-Alaoui et al., 2013) are strong evidences in favor of such approach. The magnetostatically quasistable configuration with slow averaged flow velocity can be formed in such a case.

Summary and Conclusion

In this review, we have summarized published results in which the plasma sheet in Earth’s magnetosphere has been regarded as a turbulent wake behind an obstacle formed due to high Reynolds number values. Traditional hydrodynamics shows that a turbulent wake should be formed even in the case of a laminar flow before an obstacle. In the magnetosphere, we deal not only with high Reynolds numbers, but also with the interaction between the geomagnetic field and the turbulent solar wind. These solar wind turbulent fluctuations are strongly amplified after crossing the bow shock, forming the plasma flows in the magnetosheath. Here, we have briefly summarized the results of plasma velocity and magnetic field fluctuations in the geomagnetic tail, focusing on the MHD scales, as turbulent motion on such scales makes the main contribution to the plasma transport and mixing. Despite an evident analogy between the turbulent wake behind an obstacle observed in the ordinary flows and the turbulent geomagnetic tail, this approach for the magnetospheric dynamics is not popular. In the following, we analyzed the potential reasons leading to this situation. We consider that in addition to simplicity of laminar models it is possible to identify three reasons:

• The difficulties in studies of turbulent plasma flows and especially in the detection of large vortices, even using data of multisatellite observations.

• The sheet-like structure of the plasma sheet, which is located between the tail lobes with a very low plasma density, meanwhile the ordinary turbulent wake fills up all region behind an obstacle.

• >The erroneous assumption of the mapping of the auroral oval to the plasma sheet, which contradicts the observations of nearly stationary auroral arcs during quiet periods.

In this paper, we have shown that it is possible to overcome all the above mentioned difficulties by considering the latest observational and theoretical works about the morphological mapping of the auroral oval into the equatorial plane. It is important to stress that these works showed that the main part of the auroral oval maps to the outer part of the ring current.

We analyze results of theoretical studies of tail turbulence using the results of the ideal MHD models and the model of the plasma sheet, in which regular flow across the sheet is compensated by eddy diffusion. Here we have pointed out the real advantages of such approach. We have also analyzed the main difficulties of the ideal MHD models, which commonly have not been discussed, connected to the inapplicability of the frozen-in condition. It is well known that in the magnetosphere the averaged plasma velocity is much smaller than the Alfvén velocity. In this case we cannot use the aforementioned approach and the ideal MHD cannot describe plasma systems in magnetostatic equilibrium. Nevertheless, it was possible to obtain the results of near to ideal MHD modeling reproducing the main features of plasma sheet turbulence including comparatively large-scale vortices.

The model of the plasma sheet based on the validity of the plasma and magnetic field pressure balance across the sheet is able to explain the plasma sheet thinning during substorm growth phase due to increase of the dawn-dusk electric field. This model also explains its thickening during expansion phase due to an increase in turbulence and eddy diffusion. It can also help to understand the mechanism of tail lobe filling by the plasma sheet plasma during IMF B_z > 0. Development of such mechanism permitted to predict the values of the eddy diffusion coefficients, which were obtained later experimentally, using data of ISEE-2, Interball/Tail Probe, Geotail, CLUSTER and Themis satellites. It takes away the problem of a sheet like turbulent wake behind an obstacle. Nonetheless, this model requires further development and additional verification.

Direct observations of vortices on the scales of ∼1–2 R_E showed the reliability to consider the plasma sheet as a turbulent wake behind an obstacle. We discuss a deep connection between the plasma sheet turbulence and the large-scale magnetospheric convection. This relation is analyzed with the aim to identify the vortices corresponding to the driving or integral scale of the tail turbulence. We consider that the large-scale two-vortex magnetospheric convection generated by the magnetospheric plasma pressure gradients is a real source of energy for the turbulence development and may be the driving or integral vortex of such turbulence. However, these suggestions require further investigation.

In this paper we have discussed a number of long standing magnetospheric problems, which are removed due to the existence of the turbulent plasma sheet, including the convection crisis problem. This problem ceases to exist because in case of the turbulent plasma sheet a number of particles in the magnetic flux tube is not conserved, and the approximation of adiabatic compression is not valid for the slow plasma motion. The problem of the location of the substorm expansion phase onset inside the magnetosphere at geocentric distances ∼7 R_E also obtains a reasonable explanation as the instability leading to the first auroral arc brightening can be developed only in a region which is comparatively stable before an onset.

We suggest that the long-standing problem of the role of reconnection phenomena on the magnetospheric dynamics obtain new aspect that requires additional discussion. It became clear that the reconnection phenomena are observed inside the turbulent regions and can be considered as a part of the turbulent tail dynamics.

In summary, the plasma sheet turbulence corresponds to an important part of the magnetospheric dynamics and should be studied in detail for the adequate description of the magnetospheric processes.

Author Contributions

All authors listed have made a substantial, direct, and intellectual contribution to the work and approved it for publication.

Funding

The work of MS was supported by Universidad de Santiago de Chile through the grant: DICYT N° 042031S.

Conflict of Interest

The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

Acknowledgments

We are grateful for numerous and fruitful discussions on this topic with our colleagues from the Skobeltsyn Institute of Nuclear Physics Moscow State University, the Space Research Institute RAS in Russian Federation, and the Physics Departments at the Universidad de Santiago and Universidad de Chile.

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