Articles | Volume 37, issue 5
Regular paper
10 Oct 2019
Regular paper |  | 10 Oct 2019

Strong southward and northward currents observed in the inner plasma sheet

Yan-Yan Yang, Chao Shen, and Yong Ji

It is generally believed that field-aligned currents (FACs) and the ring current (RC) are two dominant parts of the inner magnetosphere. However, using the Cluster spacecraft crossing the pre-midnight inner plasma sheet in the latitudinal region between 10 and 30 N, it is found that, during intense geomagnetic storms, in addition to FACs and the RC, strong southward and northward currents also exist which should not be FACs because the magnetic field in these regions is mainly along the xy plane. Detailed investigation shows that both magnetic-field lines (MFLs) and currents in these regions are highly dynamic. When the curvature of MFLs changes direction in the xy plane, the current also alternatively switches between being southward and northward. To investigate the generation mechanism of the southward and northward current, we employed the analysis of energetic particle flux up to 1 MeV. For energetic particles below 40 keV, observations from Cluster CIS/CODIF (Cluster Ion Spectrometry COmposition and DIstribution Function analyzer) are used. However, for higher-energy particles, the flux is obtained by extrapolations of low-energy particle data through Kappa distribution. The result indicates that the most reasonable cause of these southward and northward currents is the curvature drift of energetic particles.

1 Introduction

Abundant current systems existing in the Earth's magnetosphere play a very important role in energy transformation in different regions (Kuijpers et al., 2014). Recently, through simulations and observations, numerous studies have shown that the inner-magnetosphere currents have a more complicated structure and distribution than originally thought. For example, in the low latitude, the magnetic-field geometry can be altered significantly into a tail-like shape during storm time (Tsyganenko et al., 2003). One or multiple banana currents can exist in the inner magnetosphere, which makes the link of the current systems more complicated (Liemohn et al., 2013). In the high latitudes, field-aligned currents (FACs) have more sophisticated structures except for the known large-scale region-1 and region-2 currents (Mishin et al., 1997; Dunlop et al., 2015a, b). Therefore, more work is still needed to reveal the true nature of these current systems.

The huge progress in satellite deployments makes it possible for direct observation of the inner-magnetosphere current system. It is believed that the magnetosphere and ionosphere are linked through a ring current (RC) and FACs (e.g., Le et al., 2004; Zhang et al., 2011). Therefore, many investigations are mainly focused on these two current systems, from high (e.g., Iijima and Potemra, 1976, 1978; Wang et al., 2006; Dunlop et al., 2015a) to low latitudes (e.g., Vallat et al., 2005; Shen et al., 2014; Yang et al., 2016). The region from low to middle latitudes, which is the key area for the inner-magnetosphere current link, however, has received less attention. Graphic plots and some statistical results (e.g., Le et al., 2004) show that FACs should be the dominant current in these areas. Through Cluster satellite observations, Vallat et al. (2005) pointed out that the RC could exist at middle (or even high) latitudes. Despite the results achieved by these various research efforts, there are still no findings enabling a conclusion about the complete current morphology in low and middle latitudes. For example, are FACs and the RC the only currents in these regions? If there are other currents, what is the corresponding generation mechanism for them? To address these questions, the current distribution and magnetic-field geometry during two storm events are investigated in the latitudinal regions from 10 to 30 N.

In the following, we will use Cluster fluxgate magnetometer (FGM; Balogh et al., 1997) data to conduct the analysis for two reasons: (1) the polar orbit of Cluster offers an opportunity to go through both the low-latitude and middle-latitude regions and (2) the configuration of the four Cluster satellites makes it possible to calculate the current via Maxwell–Ampère's law and obtain the magnetic-field geometry. Moreover, in many previous works, it was thought that an asymmetric RC linked with the FACs, which is generally believed to occur during storm time, so storm events are our primary focus here.

Throughout this paper, solar magnetospheric (SM) coordinates are used. To better describe angles, spherical coordinates (θ, φ) in the SM frame are also defined; i.e., the polar angle θ (0θ180) is the angle between the +z axis and the vector direction while the azimuthal angle φ (0φ360) is rotated anticlockwise from the +x axis in the xy plane when seen from +z axis. For current density analysis, the local cylindrical coordinate system (jρ, jφ, jz; Vallat et al., 2005) is also utilized. Where jz is parallel to the +z axis, jρ represents the radial component of the current on the plane parallel to the xy plane, oriented anti-earthward; jφ points eastward, describing the RC.

2 Methodology

In this study, magnetic curvature analysis (MCA; Shen et al., 2003) and magnetic rotation analysis (MRA; Shen et al., 2007) are used; these techniques have the unique ability to reveal the three-dimensional geometric structure of the magnetic field directly as well as to provide more detailed magnetic-field-related parameters, such as the magnetic-field gradient; curvature; and the binormal of magnetic-field lines (MFLs), rotation rates, and current density. The magnetic unit vector b^=B/B, curvature vector ρc(ρc=(b^)b^), and the binormal vector N^(N^=b^×ρ^c/b^×ρ^c) are orthogonal to each other in the analysis, and the radius of curvature is Rc=1/ρc. The magnetic vector b has maximum, median, and minimum rotation rates of μ11/2, μ21/2, and μ31/2 along e^(1), e^(1), and e^(2), respectively, where e^(1), e^(1), and e^(2) are the three characteristic eigenvectors of the magnetic field. Note that because the strong geomagnetic field in the region of interest will produce artificial currents in the basic MRA calculation (nonlinear contributions), the dipole field is subtracted when using the MRA method to minimize truncation error (Shen et al., 2014).

To make a comparison with the nondisturbed geomagnetic field, the local dipolar values of the magnetic-field strength, BtDip; the radius of curvature, RcDip; the magnetic-field gradient strength, |∇BDip|; and three rotation rates, μ11/2, μ21/2, and μ31/2, are also presented. They are calculated (Shen et al., 2014) by using

(1) B tDip = M r - 3 ( 1 + 3 cos 2 θ ) , R cDip = r 3 ( 1 + 3 cos 2 θ ) 3 / [ sin θ ( 1 + cos 2 θ ) ] , B Dip = 3 M r - 4 1 + cos 2 θ ( 7 + 8 cos 2 θ ) / ( 1 + 3 cos 2 θ ) , μ 1 1 / 2 = μ θ 1 / 2 = 3 ( 1 + cos 2 θ ) / [ r ( 1 + 3 cos 2 θ ) ] , μ 2 1 / 2 = μ ϕ 1 / 2 = 3 cos θ / [ r ( 1 + 3 cos 2 θ ) ] , μ 3 1 / 2 = μ r 1 / 2 = 0 ,

where M=mμ0/4π (with m=7.78×1022A m−2 being the Earth's magnetic dipole moment) and r is the radial distance in SM coordinates.

3 Event analysis

The chosen events occurred on 12 April 2001 and 31 March 2001. These were the two largest storms from 2001 to 2004 during which the four Cluster satellites had a small (best) tetrahedron separation distance (≤1000km). The minimum Dst indices for the two events were −271 and −387nT, respectively. During the two events, Cluster was in the pre-midnight sector and traversed the RC region vertically from the Southern to Northern Hemispheres. The region of interest is in the Northern Hemisphere. Figure 1 gives the proton density and differential flux for H+, He+, and O+ during the analyzed interval, which are obtained from the Cluster Ion Spectrometer (CIS; Rème et al., 2001). The figure indicates that Cluster is mainly in the plasma sheet region (e.g., Vallat et al., 2005).

Figure 1Cluster CIS data for 12 April 2001 (left) and 31 March 2001 (right) event. (a, e) The proton density variation for three satellites: C1 (black), C3 (green), and C4 (blue). (b–d, f–h) H+, He+, and O+ energy–time spectrograms in particle flux units (ionscm-2sr-1s-1keV-1) from C4.


3.1 12 April 2001 event

The time interval of interest for the first event is from 05:00 to 05:25 UT, with latitude ranging from 16.9 to 25.7. Figure 2 presents some of the main physical quantities. Figure 2a shows the average magnetic field Bt detected from the four Cluster satellites and the local dipolar magnetic-field strength. It can be seen that the local magnetic field is enhanced in this area. Figure 2b indicates that the polar angle of the magnetic field is close to 90, showing that the magnetic field lies approximately in the xy plane. The polar angle and azimuthal angle of dipolar fields are also shown in dashed lines in Fig. 2b, which indicates a large deviation of the polar angle with observations. Figure 2c shows that the radius of curvature, Rc, has large variations. It is interesting to see that ϕc (the angle of Rc in Fig. 2d) changes direction alternately during the whole period. Therefore, eight regions (numbered from NH1 to NH8) were chosen according to the changes in the ϕc direction to investigate their features. The variations in some physical quantities are also summarized in Table 1. For ϕc and θe1, the average values (with a few large abnormal points removed) during this period are given. The “–” denotes values with large oscillations. For jz, the maximum or minimum value during each interval is presented.

Figure 2Geometry of the magnetic field and the current distribution in the Northern Hemisphere (NH) region on 12 April 2001. (a) Average magnetic strength Bt at the center of the Cluster tetrahedron (black solid line) and the calculated strength BtDip of the dipole geomagnetic field (black dashed line). (b) Direction angles (θB, ϕB) of the magnetic field. 90 and 315 are reduced respectively for θB and ϕB to better indicate the magnetic-field variation. The polar angle and azimuthal angle of dipolar fields are also show in dashed lines. (c) Radius of curvature, Rc (red solid line), and the calculated radius of curvature, RcDip, of the dipole geomagnetic field (black dashed line). (d) Direction angles (θc, ϕc) of the curvature of the MFLs. (e) Value of the gradient of magnetic-field strength for the real magnetic field (red solid line) and dipole geomagnetic field (black dashed line). (f) Direction angles (θgB, ϕgB) of the gradient of magnetic-field strength. (g) Maximum, median, and minimum rotation rates of the measured magnetic field (solid lines) and dipole geomagnetic field (dashed lines). (h) Direction angles (θe1, ϕe1) of the maximum rotation rate. (i) Total current density jt (black line) and the three components jρ (magenta line), jφ (green line), and jz (blue line) in local cylindrical coordinate system, respectively. The red line is the field-aligned component jB (red line).


As shown in Fig. 2c, the radius of curvature of MFLs in the eight regions is more varied compared with that of the dipole field. Another feature observed in Fig. 2c is that Rc peaks at the vertical dashed lines. This is reasonable, since the curvature radius in the transition region should be larger than the region where the curvature radius has opposite directions. Figure 2d and the ϕc row in Table 1 give the average value of the azimuthal direction ϕc during each interval. This quantitatively reveals that ϕc alternatively varied between 30.3 and 51.9 and 230.3 and 292.0. It is noted from Fig. 2d that, for some regions, the variation in polar angle θc has larger fluctuation (than azimuthal angle ϕc). This feature reflects larger changes of the magnetic field in z component. Figure 2g shows that μ11/2 has an enhancement in each region, illustrating a stretched MFL structure. Figure 2h and row θe1 in Table 1 show that, for most regions, the largest value of the polar angle θe1 for μ11/2 is close to 90; therefore, the largest deviation of MFLs is along the xy plane. Figure 2i indicates that the current oscillates and that the dominant current is along jρ and the north (or south) jz direction, while jφ is basically small compared with jρ and jz. To show FACs, the jB component is also given in Fig. 2i; it can be seen that the value of jB is close to that of jρ because the direction of the magnetic field points approximately to the radial direction (see Fig. 2b). The maximum values for jB and jz were ∼40 and ∼80nA m−2, respectively. From Table 1 and Fig. 2, it is interesting to see that, from region NH1 to region NH8, the jz component changed from positive (northward) to negative (southward) as ϕc varied from <50 to >230.

Table 1Variation in physical quantities for two storm events.

a Storm events considered in this work.
b The physical quantity ϕc is the average azimuthal direction of the curvature radius, θe1 is the average polar angle of maximum rotation rates of the magnetic field, and jzm represents the maximum or minimum value of the jz-current component.
c−m Regions for each storm event.

Download Print Version | Download XLSX

3.2 31 March 2001 event

Another larger storm occurred between 07:30 and 08:00 UT on 31 March 2001. The event was once reported by Shen et al. (2014), but they only concentrated on the interval from approximately 07:00 to 07:25 UT. Observations are shown in Fig. 3 for the latitudinal region from 13.1 to 31.2 N, the interval during the main phase of the storm. Here, 11 regions designated from NH1 to NH11 are divided also according to azimuthal direction changes of ϕc. The variations in some relative physical quantities are also shown in Table 1. From Fig. 3 and Table 1, it can be seen that these parameters behave the same as those of the first event, but with strong magnetic-field strength. Figure 3 indicates that the magnetic-field strength is stronger than that during the first event. The magnetic field is in the xy plane (see Fig. 3b). The radius of curvature of MFLs (see Fig. 3c), the magnetic-field gradient (Fig. 3e), and the largest rotation rate (Fig. 3g) oscillates significantly and exhibits large deviations compared with those of the dipole field. Figure 3f shows that the magnetic-field gradient is in the xy plane and directed toward the dayside. Figure 3h and row θe1 demonstrate that the largest variation in MFLs is near the xy plane. In Fig. 3i, it is clear that the jz component is the dominant current, with a maximum value of ∼300nA m−2. This value is more than triple that of the 12 April 2001 event. It is clear to see that the jφ component is the smallest among these currents. Similar to first event, jz is simultaneously observed to vary from northward to southward when φc changes direction.

Figure 3Geometry of the magnetic field and the current distribution in the NH region on 31 March 2001. The format is the same as that of Fig. 2.


4 Discussion

During the 12 April 2001 and 31 March 2001 strong storm events, the Cluster satellites were located in the pre-midnight sector and crossed from ∼10 to ∼30 N. In these regions, both the magnetic-field parameters and the current density fluctuated significantly. The MFLs, which were mainly in the xy plane, severely deviated from the dipole field and changed (stretched) along the xy plane. Figure 4 displays the total magnetic-field strength and its three components. It can be seen that the x and y components of the magnetic field have the largest fluctuations, which is consistent with the results obtained from Figs. 2 and 3. To further investigate the fluctuation, the continuous 1-D wavelet transform method is applied in the x and y component of the magnetic field. It is found that the ULF wave (ultra-low-frequency wave) covering a range of frequencies spanning from 4 to 10 mHz can be observed (not shown here), which is consistent with the typical current density variation in the ∼2–4 min period. Actually, the ULF wave in the plasma sheet region has been extensively reported in previous works (see Keiling, 2009, and references therein). Thus, it seems that ULF wave is a possible way to cause the variation in the curvature radius (and the field-aligned current).

Figure 4Magnetic field observed by the four Cluster satellites during 12 April 2001 and 31 March 2001 storm events.


The most obvious phenomenon in the two cases is the existence of three current systems, i.e., FACs, jB, an azimuthal current, jφ, and a northward (or southward) current, jz. Among them, jz is basically the strongest current component. In previous studies (e.g., Le et al., 2004; Vallat et al., 2005), the existence of jB and jφ has been proved. However, the occurrence of such a strong jz in the inner plasma sheet has not been reported before. In the work of Vallat et al. (2005), they also found a southward current (see Fig. 14 and corresponding text). But it is in the equatorial ring current region (with no direction changes) and is mainly caused by an asymmetry between the ionospheric conductivities of the two hemispheres. It is very clear that the southward current in their paper is different than what we report here.

As introduced in previous studies (e.g., Parker, 1957), the current in the inner magnetosphere generally arises from gradient drifts as well as curvature drift and the gyromotion of energetic particles. They can be calculated by using the following (e.g., Lui et al., 1987; De Michelis et al., 1999):


where j, jC, and jG represent the gradient current, curvature current, and gyromotion current, respectively, and P and P are the pressure tensor components perpendicular and parallel to the magnetic field, which can be deduced from


where m is the mass of the particle, J is the differential flux intensity, and ε and α are the particle energy and pitch angle, respectively. Since the magnetic-field gradient B and curvature ρc were obtained by using the MRA method, the above three currents can be calculated when the pressure tensor components are given.

For the two events in this study, both the magnetic field and magnetic-field gradient are directed toward the dayside. Therefore, the current deduced from B×∇B (the gradient drift current) should be small. To analyze the current contribution from gyromotion drift and curvature drift, we first show the three components of -ρc×B for the two events in Fig. 5a and b. It is clearly seen that the (-ρc×B)z component is the dominate part and has the same variation trend as jz. Therefore, the curvature drift current is a possible candidate. For gyromotion current, it originates from three terms, i.e., B×P, -B×B, and -B×(B)B. Firstly, according to previous works (e.g., Lui et al., 1987; De Michelis et al., 1999), P is along the radial direction, which means that it has a similar direction with the magnetic field to the two events analyzed here. Thus, the contribution from B×P should be small. Secondly, -B×B is similar to the gradient drift current and can be negligible. Thirdly, since (B⋅∇)B has the same direction as ρc(ρc=(b^)b^,b^=B/B), according to Fig. 5a and b, the product of -B×(B)B (similar to ρc×B) will behave oppositely to jz. Consequently, the gyromotion current has little possibility of contributing to a strong jz. According to the above analysis, the most reasonable candidate for strong jz should be the curvature drift.

Based on the above analysis, graphic plots are given in Fig. 5c and d to explain the possible generation mechanism for jz. During the strong storm time, turbulence, e.g., ULF waves, results in the fluctuation of the MFLs; then, the radius of curvature of the MFLs decreases, leading to an increase in the curvature drift current. During this process, the direction of the magnetic field is nearly unchanged because the background field is very strong. However, the curvature will alternately change directions along with the variation in the MFLs, resulting in alternating variations in -ρc×B, i.e., leading to the oscillation of jz.

Figure 5(a, b) The three components of -ρc×B for two analyzed events. ρc is calculated from MRA method, and B is the averaged magnetic field measured by four Cluster spacecraft. (c, d) Graphic plots of the origin of the jN current variation.


Figure 5a and b can only illustrate that the direction of -ρc×B is consistent with northward current. To quantitatively check if the curvature current calculated through Eq. (3) is consistent with the result obtained from the MRA method, further investigation is necessary. The CIS/CODIF (Cluster Ion Spectrometry COmposition and DIstribution Function analyzer) can provide the differential flux intensity for energy below 40 keV. Through Eqs. (3), (5), and (6), the curvature current can be estimated. The results show that the main variation trend is consistent with result from MRA, but the intensity is very small (less than 1 nA m−2; not shown here). However, it should be noted that, for Cluster CIS/CODIF, only low-energy particle data are available; therefore, a large bias may exist when calculating the storm-time current. In contrast, much higher energy is used in previous studies (e.g., 1 MeV in the work of Lui et al., 1987). Cluster RAPID can provide energy spectrograms for the high-energy particle from ∼27.6 to ∼3056keV. Unfortunately, there are no available data for the two analyzed events. The statistical study from Kronberg et al. (2015) proves that, in the near-Earth plasma sheet, higher-energy hydrogen and oxygen are greatly enhanced during geomagnetic activity. In the work of Ma et al. (2012), they also indicated that the flux for higher-energy particles could be comparable or larger than that of the low-energy particles.

Though, there is no available differential flux for high-energy particles on Cluster, the curvature current still can be estimated through simulations. Previous works have proved that the particle distribution in plasma sheet can be described as Kappa distribution functions (Pierrard and Lazar, 2010, and references therein):

(7) f = N 1 1 2 π m E 0 κ 1 2 / 3 Γ ( κ 1 + 1 ) Γ ( κ 1 - 1 / 2 ) 1 + E κ 1 E 0 - κ 1 - 1 ,

where N1 and E0 denote particle density and temperature, and κ1 is a constant. For energy satisfying EE0, Eq. (7) can be written as

(8) f = a E - κ 1 - 1 .

Since the differential flux intensity J and particle velocity distribution function f are related by J=fp2, Eq. (8) is also the function of J, namely

(9) J = a p 2 E - κ 1 - 1 ,

where p is the momentum of the concerned particles, and a is a constant. Thus, with the known differential flux intensity from low-energy particle, the parameter a and κ1 can be determined. Then, the differential flux intensity for high-energy particles (to 1 MeV) can be estimated using Eq. (9). Though particles are accelerated during the storm, we have confirmed that the Kappa distribution is still satisfied using CIS/CODIF observations (not shown here). However, it should be noted that, during the storm, a and κ1 are no longer a constant but varied with time. Besides this, to check if the estimated high-energy particle differential flux (using low-energy particle data) is reasonable, we select a storm event that occurred on 20 April 2002, which has similar position with two analyzed events in this study, and has CIS/CODIF and RAPID observations at the same time. The result shows that the fitted result (from CIS/CODIF measurement) can basically reflect the main trend of the high-energy particles, which can demonstrate that our estimation used here is reasonable. During the storm time, currents calculated via energetic particle fluxes appear to still underestimate the current. As the particle flux fit method of calculating currents works so well for earlier in the time period, this undershoot during storm time might be indicative of additional energetic particle acceleration (a harder power law) in the parallel direction. This increased parallel pressure would result in the observed larger value of jc.

Now, we can re-estimate the curvature current using Cluster CIS/CODIF observations for energy between 25 eV and 40 keV and simulation values for energy in the range >40keV–1 MeV. Figure 6 shows the estimated z component of curvature current (the red dotted curve). It is close to result from MRA (the blue curve).

Figure 6The z-component current density calculated from MRA method (the blue curve) and the estimated curvature current (the red dotted curve).


Figure 7(a, b) Cluster elongation and planarity for two studied events. The red vertical lines demarcate the analyzed time interval. Panels (c) and (d) are taken from Robert et al. (1998) to evaluate the influence of the tetrahedron shape. Black lines mark the elongation and planarity obtained from panels (a) and (b).


It should be noted that both events analyzed here are in the Northern Hemisphere. Actually, we have checked that the southward and northward current also can be observed in the southern low and middle latitudes. Thus, such currents should be observable both in northern and southern inner plasma sheet during strong geomagnetic storm events.

According to previous analysis from plasma data (Baker et al., 2002; Korth et al., 2004; Vallat et al., 2005; Ohtani et al., 2007), most NH regions should correspond to the plasma sheet region. Using the T96 model (Tsyganenko, 1995, 1996), we tried to trace Cluster footprints in the Northern Hemisphere; it is found that the position is ∼55–60 (not shown here), which just corresponds to the position of the FACs (Papitashvili et al., 2002; He et al., 2012). Because the MFL shapes in the plasma sheet were changed considerably, the particle motion in Earth's magnetic field will be altered correspondingly, which may affect the particle distribution in the polar and equatorial regions, hence leading to the variation in the FAC and RC distributions. These effects, however, need to be evaluated in future work.

When calculating current density using the MRA method, it should be noted that Cluster is not a regular tetrahedron shape around the perigee area but suffers from an elongation, which can produce an unnatural currents. These unnatural currents are included in our analysis and cannot be removed. To evaluate this component, methods from Robert et al. (1998) and Vallat et al. (2005) are used. Figure 7 gives the Cluster tetrahedron parameters for two analyzed events. Then, the current influence of the tetrahedron shape can be estimated as a function of elongation and planarity (Fig. 7c and d). It can be seen that the error caused by tetrahedron is never more than 30 %.

5 Summary

In this work, the magnetic-field geometry and current density in the inner plasma sheet during two intense geomagnetic storms were investigated. It is found that the magnetic field and current density highly fluctuated in this region. Generally, all three components of current can be observed during the analyzed interval. However, the northward (or southward) current is basically the strongest one. Detailed study shows that the MFLs align in the xy plane; thus, the northward (or southward) current should not be FACs. This property has not been reported before.

The most prominent feature of the northward (or southward) current is the alternative changing of its direction, which is found to vary simultaneously with that of the curvature. To reveal the generation mechanism of the northward (or southward) current, gradient current, curvature current, and gyromotion current are analyzed. The results show that the curvature current has the same variation trend with the northward and southward current. Then, using low-energy particle observations from Cluster CIS/CODIF, combined with simulations based on Kappa distribution, the curvature current is calculated. It shows that the estimated curvature current coincides very well with the current density directly obtained from MCA and MRA. Therefore, the curvature drift of the energetic particle is the most reasonable mechanism of the southward and northward current.

For the two events analyzed in this work, we can observe ULF waves; this is consistent with the typical current density variation period. This turbulence excited during the strong storm can result in the decrease in curvature radius and changing of direction of MFLs, then leading to an increase in the curvature currents and variation in their direction.

Data availability

Solar wind data (OMNI data set) were obtained from (last access: 22 June 2019); Cluster FGM and CIS/CODIF data were obtained, respectively, from (last access: 22 June 2019) and (last access: 22 June 2019).

Author contributions

CS was responsible for the interpretation, YJ performed the simulation, and YYY performed the data analysis and prepared the paper.

Competing interests

The authors declare that they have no conflict of interest.


We are grateful to the Cluster Science Archive, CDAWeb and OMNI for providing us with data.

Financial support

This research has been supported by the National Key R&D Program of China (grant no. 2018YFC1503501), the National Natural Science Foundation of China (grant no. 41231066), the National Natural Science Foundation of China (grant no. 41204117), and a research grant from the Institute of Crustal Dynamics, China Earthquake Administration (grant no. ZDJ2018-18).

Review statement

This paper was edited by Minna Palmroth and reviewed by two anonymous referees.


Baker D. N., Ergun, R. E., Burch, J. L., Jahn, J. M., Daly, P. W., Friedel, R., Reeves, G. D., Fritz, T. A., and Mitchell, D. G.: A telescopic and microscopic view of a magnetospheric substorm on 31 March 2001, Geophys. Res. Lett., 29, 1862,, 2002. 

Balogh, A., Dunlop, M. W., Cowley, S. W. H., Southwood, D. J., Thomlinson, J. G., Glassmeier, K. H., Musmann, G., Luhr, H., Buchert, S., Acuna, M. H., Fairfield, D. H., Slavin, J. A., Riedler, W., Schwingenschuh, K., and Kivelson, M. G.: The Cluster magnetic field investigation, Space Sci. Rev., 79, 65–91,, 1997. 

De Michelis, P., Daglis, I. A., and Consolini, G.: An average image of proton plasma pressure and of current systems in the equatorial plane derived from AMPTE/CCE-CHEM measurements, J. Geophys. Res., 104, 28615–28624,, 1999. 

Dunlop, M. W., Yang, Y. Y., Yang, J. Y., Lühr, H., Shen, C., Olsen, N., Ritter, P., Zhang, Q. H., Cao, J. B., Fu, H. S., and Haagmans, R.: Multispacecraft current estimates atswarm, J. Geophys. Res.-Space Phys., 120, 8307–8316,, 2015a. 

Dunlop, M. W., Yang, J. Y., Yang, Y. Y., Xiong, C., Lühr, H., Bogdanova, Y. V., Shen, C., Olsen, N., Zhang, Q. H., Cao, J. B., Fu, H. S., Liu, W. L., Carr, C. M., Ritter, P., Masson, A., and Haagmans, R.: Simultaneous field-aligned currents at Swarm and Cluster satellites, Geophys. Res. Lett., 42, 3683–3691,, 2015b. 

He, M., Vogt, J., Lühr, H., Sorbalo, E., Blagau, A., Le, G., and Lu, G.: A high-resolution model of field-aligned currents through empirical orthogonal functions analysis (MFACE), Geophys. Res. Lett., 39, L18105,, 2012. 

Iijima, T. and Potemra, T. A.: Field-aligned currents in the dayside cusp observed by Triad, J. Geophys. Res., 81, 5971,, 1976. 

Iijima, T. and Potemra, T. A.: Large-scale characteristics of field-aligned currents associated with substorms, J. Geophys. Res., 83, 599–615,, 1978. 

Keiling, A.: Alfvén waves and their roles in the dynamics of the Earth's magnetotail: A review, Space Sci. Rev., 142, 73–156,, 2009. 

Korth, A., Fränz, M., Zong, Q. G., Fritz, T. A., Sauvaud, J. A., Rème, H., Dandouras, I., Friedel, R., Mouikis, C. G., Kistler, L. M., Möbius, E., Marcucci, M. F., Wilber, M., Parks, G., Keiling, A., Lundin, R., and Daly, P. W.: Ion injections at auroral latitude during the March 31, 2001 magnetic storm observed by Cluster, Geophys. Res. Lett., 31, L20806,, 2004. 

Kronberg, E. A., Grigorenko, E. E., Haaland, S. E., Daly, P. W., Delcourt, D. C., Luo, H., Kistler, L. M., and Dandouras, I.: Distribution of energetic oxygen and hydrogen in the near-Earth plasma sheet, J. Geophys. Res.-Space Phys., 120, 3415–3431,, 2015. 

Kuijpers, J., Frey, H., and Fletcher, L.: Electric Current Circuits in Astrophysics, Space Sci. Rev., 188, 1–55, 2014. 

Le, G., Russell, C. T., and Takahashi, K.: Morphology of the ring current derived from magnetic field observations, Ann. Geophys., 22, 1267–1295,, 2004. 

Liemohn, M. W., Ganushkina, N. Y., Katus, R. M., De Zeeuw, D. L., and Welling, D. T.: The magnetospheric banana current, J. Geophys. Res.-Space Phys., 118, 1–13,, 2013. 

Lui, A. T. Y., McEntire, R. W., and Krimigis, S. M.: Evolution of the ring current during two geomagnetic storms, J. Geophys. Res., 92, 7459–7470,, 1987. 

Ma, Y., Shen, C., Angelopoulos, V., Lui, A. T. Y., Li, X., Frey, H. U., Dunlop, M., Auster, H. U., McFadden, J. P., and Larson, D.: Tailward leap of multiple expansions of the plasma sheet during a moderately intense substorm: THEMIS observations, J. Geophys. Res., 117, A07219,, 2012. 

Mishin, V. M., Block, L. P., Bazarzhapov, A. D., Saifudinova, T. I., Lunvushkin, S. B., Shirapov, D. S., Woch, J., Eliasson, L., Marklund, G. T., Biotaberg, L. G., and Opgenoor, H.: A study of the CDAW 9C substorm of May 3, 1986, using magnetograrn inversion technique 2, and a substorm scenario with two active phases, J. Geophys. Res., 102, 19845–19859,, 1997. 

Ohtani, S., Korth, H., Brandt, P. C., Blomberg, L. G., Singer, H. J., Henderson, M. G., Lucek, E. A., Frey, H. U., Zong, Q., Weygand, J. M., Zheng, Y., and Lui, A. T. Y.: Cluster observations in the inner magnetosphere during the 18 April 2002 sawtooth event: Dipolarization and injection at r=4.6RE, J. Geophys. Res., 112, A08213,, 2007. 

Papitashvili, V. O., Christiansen, F., and Neubert, T.: A new model of field-aligned currents derived from high-precision satellite magnetic field data, Geophys. Res. Lett., 29, 1683,, 2002. 

Parker, E. N.: Newtonian development of the dynamical properties of ionized gases of low density, Phys. Rev., 107, 924–933, 1957. 

Pierrard, V. and Lazar, M.: Kappa distributions: Theory and applications in space plasmas, Solar Phys., 267, 153–174,, 2010. 

Rème, H., Aoustin, C., Bosqued, J. M., Dandouras, I., Lavraud, B., Sauvaud, J. A., Barthe, A., Bouyssou, J., Camus, Th., Coeur-Joly, O., Cros, A., Cuvilo, J., Ducay, F., Garbarowitz, Y., Medale, J. L., Penou, E., Perrier, H., Romefort, D., Rouzaud, J., Vallat, C., Alcaydé, D., Jacquey, C., Mazelle, C., d'Uston, C., Möbius, E., Kistler, L. M., Crocker, K., Granoff, M., Mouikis, C., Popecki, M., Vosbury, M., Klecker, B., Hovestadt, D., Kucharek, H., Kuenneth, E., Paschmann, G., Scholer, M., Sckopke, N., Seidenschwang, E., Carlson, C. W., Curtis, D. W., Ingraham, C., Lin, R. P., McFadden, J. P., Parks, G. K., Phan, T., Formisano, V., Amata, E., Bavassano-Cattaneo, M. B., Baldetti, P., Bruno, R., Chionchio, G., Di Lellis, A., Marcucci, M. F., Pallocchia, G., Korth, A., Daly, P. W., Graeve, B., Rosenbauer, H., Vasyliunas, V., McCarthy, M., Wilber, M., Eliasson, L., Lundin, R., Olsen, S., Shelley, E. G., Fuselier, S., Ghielmetti, A. G., Lennartsson, W., Escoubet, C. P., Balsiger, H., Friedel, R., Cao, J.-B., Kovrazhkin, R. A., Papamastorakis, I., Pellat, R., Scudder, J., and Sonnerup, B.: First multispacecraft ion measurements in and near the Earth's magnetosphere with the identical Cluster ion spectrometry (CIS) experiment, Ann. Geophys., 19, 1303–1354,, 2001. 

Robert, P., Dunlop, M. W., Roux, A., and Chanteur, G.: Accuracy of current density determination, in Analysis Methods for Multi-Spacecraft data, ISSI Sci. Rep., SR-001, 395–418, 1998. 

Shen, C., Li, X., Dunlop, M., Liu, Z. X., Balogh, A., Baker, D. N., Hapgood, M., and Wang, X.: Analyses on the geometrical structure of magnetic field in the current sheet based on cluster measurements, J. Geophys. Res., 108, 1168,, 2003. 

Shen, C., Li, X., Dunlop, M., Shi, Q. Q., Liu, Z. X., Lucek, E., and Chen, Z. Q.: Magnetic field rotation analysis and the applications, J. Geophys. Res., 112, A06211,, 2007.  

Shen, C., Yang, Y. Y., Rong, Z. J., Li. X., Dunlop, M., Carr, C. M., Liu, Z. X., Baker, D. N., Chen, Z. Q., Ji, Y., and Zeng, G.: Direct calculation of the Ring Current distribution and magnetic structure seen by Cluster during Geomagnetic Storms, J. Geophys. Res.-Space Phys., 119, 2458–2465,, 2014. 

Tsyganenko, N. A.: Modeling the Earth's magnetospheric magnetic field, confined within a realistic magnetopause, J. Geophys. Res., 100, 5599–5612, 1995. 

Tsyganenko, N. A.: Effects of the solar wind conditions on the global magnetospheric configuration as deduced from data-based field models, in: Proceedings of the Third International Conference on Substorms (ICS-3), Versailles, France, 12–17 May 1996, edited by: Rolfe, E. and Kaldeich, B., Eur. Space Agency Spec. Publ., ESA-SP, 389, 181–185, 1996. 

Tsyganenko, N. A., Singer, H. J., and Kasper, J. C.: Storm-time distortion of the inner magnetosphere: How severe can it get?, J. Geophys. Res., 108, 1209,, 2003. 

Vallat, C., Dandouras, I., Dunlop, M., Balogh, A., Lucek, E., Parks, G. K., Wilber, M., Roelof, E. C., Chanteur, G., and Rème, H.: First current density measurements in the ring current region using simultaneous multi-spacecraft CLUSTER-FGM data, Ann. Geophys., 23, 1849–1865,, 2005. 

Wang, H., Lühr, H., Ma, S. Y., Weygand, J., Skoug, R. M., and Yin, F.: Field-aligned currents observed by CHAMP during the intense 2003 geomagnetic storm events, Ann. Geophys., 24, 311–324,, 2006. 

Yang, Y. Y., Shen, C., Dunlop, M., Rong, Z. J., Li, X., Angelopoulos, V., Chen, Z. Q., Yan, G. Q., and Ji, Y.: Storm time current distribution in the inner equatorial magnetosphere: THEMIS observations, J. Geophys. Res.-Space Phys., 121, 5250–5259,, 2016. 

Zhang, Q.-H., Dunlop, M. W., Lockwood, M., Holme, R., Kamide, Y., Baumjohann, W., Liu, R.-Y., Yang, H.-G., Woodfield, E. E., Hu, H.-Q., Zhang, B.-C., and Liu, S.-L.: The distribution of the ring current: Cluster observations, Ann. Geophys., 29, 1655–1662,, 2011. 

Short summary
Previous studies show that the ring current (RC) and field-aligned currents (FACs) are the dominant currents in the inner magnetosphere. However, through two large storm events observed by Cluster, we find new strong southward and northward currents in the latitudinal region from 10° N to 30° N. Theoretical analysis indicates that these currents originated from the fluctuation of magnetic field lines during strong geomagnetic storms.