ORIGINAL RESEARCH article
Energy Conversion at Kinetic Scales in the Turbulent Magnetosheath
- 1Space Research Institute, Austrian Academy of Sciences, Graz, Austria
- 2Geodetic and Geophysical Institute, Hungarian Academy of Sciences, Sopron, Hungary
- 3Swedish Institute of Space Physics, Uppsala, Sweden
The process of conversion or dissipation of energy in nearly collisionless turbulent space plasma, is yet to be fully understood. The existing models offer different energy dissipation mechanisms which are based on wave particle interactions or non-resonant stochastic heating. There are other mechanisms of irreversible processes in space. For example, turbulence generated coherent structures, e.g., current sheets are ubiquitous in the solar wind and quasi-parallel magnetosheath. Reconnecting current sheets in plasma turbulence are converting magnetic energy to kinetic and thermal energy. It is important to understand how the multiple (reconnecting) current sheets contribute to spatial distribution of turbulent dissipation. However, detailed studies of such complex structures have been possible mainly via event studies in proper coordinate systems, in which the local inflow/outflow, electric and magnetic field directions, and gradients could be studied. Here we statistically investigate different energy exchange/dissipation (EED) measures defined in local magnetic field-aligned coordinates, as well as frame-independent scalars. The presented statistical comparisons based on the unique high-resolution MMS data contribute to better understanding of the plasma heating problem in turbulent space plasmas.
Turbulence represents an unsolved problem in classical physics of continuous media (e.g., fluids) characterized by velocity shears, intermittent distribution of kinetic energy over multiple spatial, and temporal scales involving strong non-linear interactions and many (possibly infinite) degrees of freedom (e.g., Frisch, 1995). Natural fluid or gaseous flows have both laminar and turbulent components. Some examples are the atmospheric/oceanic circulation, the blood flow, turbulent river flows, turbulent flows in engineering, industrial and laboratory settings, etc. In natural and artificial flows the turbulence strength usually plays a decisive role determining the overall dynamical behavior of a given system. Turbulence in astrophysical systems is also expected to affect the dynamical behavior of plasmas over multiple scales, for example, modifying transport processes or supporting large-scale instabilities (Brandenburg and Lazarian, 2013). On the Sun, among others, turbulence can play a role in coronal heating, solar wind expansion (Cranmer et al., 2015) and particle acceleration (Vlahos et al., 2019). In-situ observations of solar wind fluctuations near the ecliptic and at high latitudes revealed scaling and intermittency features resembling the large-scale properties of hydrodynamic turbulence (Tu and Marsch, 1995; Bruno and Carbone, 2013). Within the terrestrial magnetosphere, because of the limited volumes and boundaries, the large fluid-scale scaling features of turbulent fluctuations might be less accessible (Vörös et al., 2007). Nevertheless, plasma turbulence in the geospace environment also plays a significant role in plasma transport and energization (Borovsky and Funsten, 2003; Vörös et al., 2006; Zimbardo et al., 2010). Space plasma turbulence significantly differs from neutral fluid turbulence in several aspects. It contains a magnetic field which introduces anisotropies into turbulent fluctuations and it is nearly collisionless. In the absence of collisions the dissipation of energy and heating of plasma is rather different from the collisional dissipation in neutral fluids (Howes et al., 2008; Alexandrova et al., 2013; Parashar et al., 2015). The basically collisionless energy transfer processes at kinetic scales happen through wave-field-fluctuation particle interactions, including Landau damping (Chen et al., 2009; Schekochihin et al., 2009), cyclotron damping (Hollweg and Markovskii, 2002) and stochastic heating (Chandran et al., 2010; Hoppock et al., 2018; Schekochihin et al., 2018). Particle energization and heating can happen at (reconnecting) current sheets (Dmitruk et al., 2004; Retino et al., 2007; Servidio et al., 2009; Osman et al., 2012) generated by turbulence through self-organization (Matthaeus et al., 2015). Current sheets observed in the turbulent solar wind (Greco et al., 2009; Servidio et al., 2011) and in the turbulent magnetosheath downstream of a quasi-parallel shock (Chasapis et al., 2015; Vörös et al., 2016; Stawarz et al., 2019) are ubiquitous.
In this paper, using high-resolution field and plasma data from the Magnetospheric Multi-Scale (MMS) mission we investigate derived energy exchange/dissipation measures at (reconnecting) current sheets in the turbulent quasi-parallel magnetosheath. The paper is organized as follows. Section 2 explains the data and instrumentation and section 3 introduces the EED measures and their time evolution during a more than 4 min long time interval in the turbulent magnetosheath. Section 4 presents a conditional statistics of averaged EED measures for normalized current densities. Section 5 contains the summary and conclusions.
2. Data and Instrumentation
We consider the time interval between 00:21:45 and 00:26:15 UT on November 30, 2015, when the MMS spacecraft were in the strongly compressed quasi-parallel magnetosheath. The MMS fleet was at the GSE position (9, –3, –0.5) RE in tetrahedron configuration with inner probe separation between 4 and 22 km comparable to the electron and ion inertial lengths of ~1 and 20 km, respectively. During the selected time interval the ion and electron moments with time resolution of 150 and 30 ms, respectively, are available from Fast Plasma Investigation (FPI) instrument (Pollock et al., 2016). The electric field data from Electric Double Probes (EDP) instrument are available with time resolution of 8 kHz (Ergun et al., 2016; Lindqvist et al., 2016; Torbert et al., 2016b). The merged digital fluxgate (FGM) (Russell et al., 2016) and search coil (SCM) (Contel et al., 2016) data were developed by using instrument frequency and timing models that were created during the FIELDS integration test campaign (Fischer et al., 2016; Torbert et al., 2016b). The merged magnetic data analyzed here consists of FGM measurements below 4 Hz and data from SCM between 1 Hz and 6 kHz.
Figure 1 contains the field and plasma data for the selected period of time. Figures 1A,E show the GSE components of the magnetic field and of the electric field from MMS1 spacecraft. Figures 1B–D are quantities calculated from multi-point spacecraft measurement. Figure 1B contains the magnetic shear angles θij obtained between spacecraft pairs MMS2-1, 3-1, and 4-1. Figures 1C,D show the magnitude of the magnetic field curvature (curvB) and curlometer current density (Jcurl) GSE components, calculated by using the well-known four-point techniques (Dunlop et al., 1988; Chanteur, 1998). The rest of the subplots show electron (Figures 1F–H) and ion (Figures 1I–K) omnidirectional differential energy flux spectrograms, temperature (including parallel and perpendicular values to the magnetic field) and velocity data, respectively. All parameters show high variability, including the electron and ion energy flux spectrograms. The electron velocity (Figure 1H) fluctuates more than the ion velocity (Figure 1K), which indicates the presence of electron scale structures in the magnetosheath. The temperature anisotropy is stronger for the electrons (Figure 1G) than for the ions (Figure 1J), showing preferential electron heating in the parallel direction.
Figure 1. Overview of the event. (A) magnetic field components in GSE (BX, BY, BZ); (B) magnetic shear angle between spacecraft pairs θ; (C) magnetic field curvature curvB; (D) curlometer current density components in GSE (JX, JY, JZ) (E) electric field components in GSE (EX, EY, EZ); (F) omnidirectional electron differential energy flux spectrogram; (G) electron temperature (Te), parallel (Te‖) and perpendicular (Te⊥) to magnetic field electron temperatures; (H) electron velocity components in GSE (VeX, VeY, VeZ); (I) omnidirectional ion differential energy flux spectrogram; (J) ion temperature (Ti), parallel (Ti‖) and perpendicular (Ti⊥) to magnetic field ion temperatures; (K) ion velocity components in GSE (ViX, ViY, ViZ).
On the X axis of Figure 1G four time intervals are highlighted: (a) Quiet interval (after 00:22:18 UT indicated by brown color) when θij, curvB, E, and Jcurl are small, which means that the spacecraft do not cross any current sheets; (b) Time interval 1 (red color), the enhanced currents, magnetic shear and curvature are associated with reconnecting current sheet exhibiting a full set of fluid and kinetic scale signatures of magnetic reconnection (Vörös et al., 2017); (c) Time interval 2 (red color) contains a strong current sheet associated with electron acceleration parallel to the magnetic field, without clear signatures of ongoing reconnection (Eriksson et al., 2016); (d) Time interval 3 (red color), here ion and electron scale signatures of magnetic reconnection (Yordanova et al., 2016). During the studied active time intervals 1–3 localized enhancements of electron and proton temperatures were also observed. From the ion energy flux spectrogram (Figure 1I), it is also visible that occasionally the most energetic ions appear first, such dispersed ion can be generated by remote sources (Vörös et al., 2017). Such dispersion features in the electron energy flux spectrogram are not seen (Figure 1F). Relative to the currents in the quiet time interval there are multiple enhancements of the current density frequently associated with rotation of the magnetic field and enhanced curvB (Figures 1B–D). Therefore, it is meaningful to further investigate how these current structures are associated with energy conversion/dissipation processes.
3. EED (Energy Exchange/Dissipation) Measures
The electron momentum equation in a two-fluid collisionless plasma can be expressed in the form (Gurnett and Bhattacharjee, 2005):
where is the electric field in the moving frame of electrons, ℙe is the electron pressure tensor, N is the plasma density and the last term which is proportional to the mass of electrons (me), the electron inertia term, is negligible when the spatial scale lengths are greater than the electron inertial length. Since collisionless reconnection is associated with multi-scale physics, the ion and electron scales are important in describing the electric fields and currents. In this paper we neglect the last term in Equation (1) and we consider the two remaining terms for constructing the EED measures:
which correspond to the rate of work done by non-ideal part of electric field on plasma particles. Here ∇.ℙe was again calculated by using the four-point techniques (Chanteur, 1998). Both quantities are used in studies of energy conversion rates associated with magnetic reconnection (e.g., Burch et al., 2016; Torbert et al., 2016a). However, the energy exchange processes in turbulent collisionless plasmas can be more complicated. Recent particle in cell simulations indicate that the pressure-stress interactions can also channel the energy of turbulent fluid motions to plasma particles and this type of energy transfer is preferentially localized at coherent structures (Yang et al., 2017). A recent study by Chasapis et al. (2018) has suggested that perhaps both channels of energy conversion, the work by electromagnetic fields and the effects of pressure-stress interactions can be analyzed by using the high resolution MMS data. The pressure-stress interactions describe the transfer of energy from multi-scale fluid motions (possibly via a turbulent cascade) to thermal energy and depend on the pressure tensor and velocity gradients. While this energy conversion channel can also be important in collisionless space plasmas (Chasapis et al., 2018), we believe more studies would be needed to optimize the multi-spacecraft separations to properly estimate the underlying scales and velocity gradients. In this paper the pressure-stress terms are not considered. On the other hand, we also consider the frame independent measure introduced by Zenitani et al. (2011):
which is similar to Equation (2), however, Equation (4) contains the additional second term on the right side corresponding to the work associated with the transport of net charge. For the time interval considered here the mean value of this term is ~ 0 nW/m3 with dispersion of ~ 0.7 nW/m3 (not shown). We note that the average values of electron and ion densities are rather high and approximately equal to ~ 100 1/cm3, therefore the plasma moments are well determined.
Figures 2A,B contain the magnetic field and curlometer current density components. In Figures 2C–G the non-ideal electric field components and the EED measures (Equations 2–4) are shown. Since the goal is to perform a statistical analysis, the field-aligned coordinate system (FAC) is chosen in which the currents, electric fields and the derived measures are transformed to parallel and two perpendicular components relative to the local mean magnetic field. Before calculating the EED measures the electric fields were filtered using a fourth-order elliptic low-pass filter. This removes the high-frequency part of the electric field fluctuations over 1 Hz which can be associated with electrostatic noise or waves. In this way, also the unpredictable effect of stochastic high-frequency fluctuations of the electric field on the dot products in Equations (2–4) is reduced. Since the field aligned and field perpendicular EED measures can be associated with different physical processes (Ergun et al., 2018), in calculating the dot products the parallel and perpendicular components of currents and electric fields are taken, for example, and . To make the calculations possible for the whole time interval the perpendicular directions 1 and 2 are not distinguished.
Figure 2. (A) magnetic field components in GSE (BX, BY, BZ); (B) curlometer current density components in field-aligned (FAC) coordinates (J⊥1, J⊥2, J‖); (C) electric field in the moving electron frame in FAC coordinates; (D) electric field calculated from the divergence of electron pressure tensor (E∇.Pe) in FAC coordinates; (E–G) EED measures; (E) J.E′ and the perpendicular and parallel products (Equation 2); (F) and the perpendicular and parallel products (Equation 3); (G) De (Equation 4).
Figure 2 demonstrates that during the quiet time interval (after 00:22:18 UT, indicated in Figure 2G), in the absence of current structures, the EED measures (Figures 2E–G) remain close to zero. The previously reported (reconnecting) current sheet events, time intervals 1,2,3, are all associated with elevated values of EED measures. The largest deviations of the measures are associated with the strongest currents during the event 2.
Figures 3A–C show the histograms of the EED measures, separately for the dot products (blue color), the perpendicular (green color) and the parallel (red color) products, respectively. Data for MMS3 spacecraft are shown. The broader distribution corresponds to J.E′ as it is larger over the sub-ion scales than and also it does include some contributions from the fluid scale stresses. For each subplot and product type the skewness of the distributions are shown on the right. The positive skewness means that the distributions have longer tails in positive direction with the meaning that there might exist a net dissipation in the overall energy exchange processes in the turbulent magnetosheath. The largest skewness are associated with EED measures in parallel to magnetic field direction.
Figure 3. (A–C) Histograms of EED measures and their perpendicular and parallel products from MMS3 sapcecraft; The color coded skewness associated with a histogram is shown for each component on the right.
4. Conditional Statistics
The goal of the paper is to determine how the local dissipation depends on the strength of the current density in turbulence. To this end we calculated the time averaged EED measures conditioned on current density and normalized to the time averages of the same measure over the whole time interval. In other words, the relative local enhancements of EED measures for certain values of current densities are estimated relative to the background fluctuations of EED measures, for examples < J.E′|J > / < J.E′ >. These quantities are plotted against the normalized current density |J|/|J|rms ≡ J/Jrms, where Jrms is the root mean square. For each EED measure and MMS1-4 spacecraft the parallel (triangles) and the perpendicular components (circles) of the dot products are shown in Figures 4A–C. Again, in dependence on J/Jrms the measures in parallel direction grow faster. The dependence of normalized EED measures averaged in time and over the spacecraft are shown with thick black lines in each subplot. For comparison, in Figure 4C the results from 2.5D PIC (magenta color) and 3D PIC (green color) are also shown (Wan et al., 2015). It can be seen that in simulations the normalized conditional average < De|J > increases faster with J than in the magnetosheath turbulence. However, there is a qualitative agreement, showing that stronger current densities are associated with larger dissipation. This seems to be a valid statement for each EED measure.
Figure 4. (A–C) Normalized current density J/Jrms (rms = root mean square) versus conditional temporal averages of normalized EED measures calculated by conditioning on the values of current density J. The color code in each subplot corresponds to the spacecraft MMS1-4. The triangles show the parallel and the circles the perpendicular products. The thick black lines represent temporal and spatial averages between MMS1-4. In subplot (C) the results from 2.5D and 3D PIC simulations are shown (Wan et al., 2015).
In Figure 4 the EED measures start increasing roughly at J = 3Jrms and there are significant differences between components and spacecraft. Actually, Jrms ~ 0.6 μA/m2 and for e.g., 4Jrms the threshold for J is 2.4 μA/m2 which corresponds to only a few current sheets in Figure 2B. For J = 6Jrms = 3.6 μA/m2 it is only one current sheet (event 2 in Figure 2B) which enters into the statistics in Figure 4, therefore the differences between the spacecraft can be understood as due to different crossing geometries across the same event.
5. Summary and Conclusions
In this study more than 4 min of high resolution field and plasma data from the MMS spacecraft was analyzed. Although longer time intervals of magnetosheath data were available from the previous missions, the time resolution of the plasma data was not sufficient to study the thin structures generated by turbulence. The measures corresponding to the work done by electric fields (J.E′ and ) and the corrected measure obtained after removing the net charge transport term (De), were estimated. The statistical analysis of the temporally and spatially averaged and normalized measures has shown that there is a net irreversible work done by electric fields at current sheets. The averaged < De|J > increases as the current density increases in qualitative agreement with PIC numerical simulations (Wan et al., 2015). However, the time interval under study is rather short when currents stronger than 5 − 6Jrms are considered for statistical analysis.
The relative importance of the terms in Equation (1) and of the EED measures in Equations (2–4) have been studied both numerically and experimentally at reconnecting current sheets (Hesse et al., 2016; Nakamura et al., 2016; Shay et al., 2016; Torbert et al., 2016b; Genestreti et al., 2018). According to these event studies, E′ (left hand side of Equation 1) dominates outside the reconnection diffusion region, where both electrons and ions are attached to the magnetic field, and the right hand side of the Equation (1) is negligible. Inside the electron diffusion region, where both ions and electrons are demagnetized, the terms on the right hand side of Equation (1) balance E′ and the first term on the right, (∇.ℙe), is much larger than the second inertial term. However, near the reconnection X-line the inertial term can reach half of the pressure divergence term (Genestreti et al., 2018). Since the probability of crossing multiple reconnection X-lines in the magnetosheath is low, the inertial term can be neglected. On the other hand, in terms of EED measures (Equations 2–4), enhanced energy conversion/dissipation can occur not only within the electron diffusion region, but also at reconnection separatrices (Shay et al., 2016). Obviously, when the focus is on understanding of the statistics of dissipation occurring at multiple current sheets in the turbulent magnetosheath the geometry of crossings or the proper coordinate systems of local current sheets cannot be controlled. Our results show that in the quasi-parallel magnetosheath the electric fields (left and right hand sides of Equation 1) and the EED measures are intermittently enhanced. At the same time (Figures 2C,D) and except for the current sheet during time interval 2, (Figures 2E–G, 3). The comparison of histograms in Figures 3A,C shows that the distribution of De is narrower than the distribution of J.E′, moreover, the tails of the histograms are also different. However, the comparison of the averaged and normalized EED measures at current sheets in Figure 4 shows that, for stronger currents, De is slightly larger than J.E′. The EED measures with net positive kurtosis (Figure 3) and irreversible work at current sheets (Figure 4) indicate that the spacecraft are crossing ion-electron scale current structures, reconnecting current sheets or reconnection separatrices in the turbulent magnetosheath. In fact, case studies have already shown that during the time interval 2 the MMS spacecraft touched the outer electron diffusion region (Vörös et al., 2017) and during the time interval 3 MMS went through a reconnection separatrix (Yordanova et al., 2016).
It was also found that during the analyzed time interval dissipation occurred preferentially in parallel direction to the magnetic field. This is seen in Figure 1G, where Te‖ > Te⊥, but mainly in Figures 3, 4, where the statistics of EED measures is presented. In a similar study by Ergun et al. (2018) it was found that the net dissipation in the Earth's plasma sheet was mainly associated with the perpendicular contribution of J.E′ and the parallel part represented merely 20% of dissipation. However, Ergun et al. (2018) did not apply any conditioning on current sheets for their EED measure. Also, on the basis of Cluster observations of magnetic reconnection in the Earth's magnetotail (Fu et al., 2017) found that in terms of J.E′ > 0 energy dissipation occurred at current filaments, at spiral nulls (O-lines) mainly in perpendicular direction to the magnetic field. However, near radial nulls (X-lines) energy dissipation was surprisingly small. Although in our case the dissipation occurred mainly in the parallel to magnetic field direction, at some MMS spacecraft the EED measures also show net positive dissipation in perpendicular direction as well. Again, in a statistical analysis which includes multiple current sheets the crossings of particular locations of the underlying structures cannot be controlled. Also, the magnetic shear angles (<180°) in Figure 1B indicate, that at least over the MMS separation distances, the magnetic field associated with the current sheets is not fully antiparallel and significant guide fields can exist. A reconnection event study has shown that the guide field during time interval 1 reached ~20% of the main magnetic field (Vörös et al., 2017). Recently, in a statistical study of magnetic reconnection events in the turbulent magnetosheath, Phan et al. (2018) have shown that out of 34 events 23 were associated with magnetic shear angles <45°. We can speculate that in turbulent space plasmas the chaotic motions typically generate current sheets with significant guide fields. Both numerical simulations (Shay et al., 2014) and data analysis (Phan et al., 2013; Wilder et al., 2018) show that a guide field suppresses electron perpendicular heating and supports parallel heating. This could explain our observations of preferred parallel heating and energy conversion at magnetosheath current sheets.
Although our understanding of the energy conversion mechanisms at current sheets has improved over the past years, we are far from seeing the complete picture of the associated turbulent dissipation. We mention here two limiting factors. First, the generating mechanisms of current sheets and the role of velocity gradients needs to be understood better. Second, reconnecting current sheets in 3D turbulence can be associated with electron scale coherent structures, for example, interacting extended flux ropes (Daughton et al., 2011). In both cases the one-scale tetrahedron geometry (Cluster or MMS) appears to be a limiting factor in the observation of real multi-scale 3D processes.
Certainly, further numerical simulations, event studies and statistical analysis of current sheets will be needed to understand better the role of coherent structures in kinetic energy conversions in collisionless turbulent plasmas and their contribution to the total heating of larger plasma volumes.
The datasets analyzed for this study can be found in the MMS science data archive https://lasp.colorado.edu/mms/sdc/public/.
ZV and EY analyzed the data and drafted the manuscript. YK, AV, and YN contributed to the interpretation of the analysis and general improvements in the manuscript.
ZV was supported by the Austrian FWF project P28764-N27. EY was supported by the Swedish Civil Contingencies Agency, grant 2016-2102.
Conflict of Interest Statement
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.
We are grateful for numerous discussions on this topic with R. Nakamura and O. W. Roberts, both from Space Research Institute, Graz.
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Keywords: plasma turbulence, current sheets, magnetic reconnection, terrestrial magnetosheath, plasma heating
Citation: Vörös Z, Yordanova E, Khotyaintsev YV, Varsani A and Narita Y (2019) Energy Conversion at Kinetic Scales in the Turbulent Magnetosheath. Front. Astron. Space Sci. 6:60. doi: 10.3389/fspas.2019.00060
Received: 30 June 2019; Accepted: 30 August 2019;
Published: 13 September 2019.
Edited by:Antonella Greco, Department of Physics, University of Calabria, Italy
Reviewed by:Yan Yang, Southern University of Science and Technology, China
Anton Artemyev, Space Research Institute (RAS), Russia
Copyright © 2019 Vörös, Yordanova, Khotyaintsev, Varsani and Narita. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
*Correspondence: Zoltán Vörös, firstname.lastname@example.org