In this paper, the anisotropic nature of the magnetic turbulence associated with magnetic dipolarizations in the Earth’s plasma sheet is examined. Specifically, we determine the power spectral indices for the perpendicular and parallel components of the fluctuating magnetic field with respect to the background magnetic field, and compare them in order to identify possible anisotropic features. For this study, we identify a total of 47 dipolarization events in February 2008 using the magnetic field data observed by the THEMIS A, D and E satellites when they are situated near the neutral sheet in the nearEarth tail. For the identified events, we estimate the spectral indices for the frequency range from 1.3 mHz to 42 mHz. The results show that the degree of anisotropy, as defined by the ratio of the spectral index of the perpendicular components to that of the parallel component, can range from ~0.2 to ~2.6, and there are more events associated with the ratio greater than unity (i.e., the perpendicular index being greater than the parallel index) than those which are anisotropic in the opposite sense. This implies that the dipolarizationassociated turbulence of the magnetic field is often anisotropic, to some nonnegligible degree. We then discuss how this result differs from what the theory of homogeneous, anisotropic, magnetohydrodynamic turbulence would predict.
1. INTRODUCTION
Magnetic field dipolarization is a sudden change of the magnetic field structure from a stretched configuration(taillike) to a dipolar configuration in the magnetotail, and is usually observed associated with substorm occurrence in the Earth’s magnetosphereionosphere system(Park et al. 2010). Often, the dipolarization process is characterized by complex fluctuations, the turbulent nature of which has only been studied to a limited extent.Magnetic turbulence is important because it could possibly influence the transport and acceleration of plasma particles in association with substorms, and could shed some light on related plasma instabilities, the details of which, however, are largely unknown. The origin of such turbulence is also a fundamental question, as it can be due either to internal instabilities in the nearEarth tail, or to flow activities associated with midtail magnetic reconnection.
There are several papers on turbulence in the Earth’s plasma sheet. A preliminary assessment on turbulence in the Earth’s plasma sheet was made by Borovsky et al.(1997). The study included an overall description on a variety of aspects of turbulence in the plasma sheet, but detailed explanations on many issues were left unanswered.Borovsky & Funsten (2003) later extended the work to achieve an improved understanding of turbulence in the plasma sheet. Both papers include discussions on turbulence of both plasma flows and the magnetic field. Angelopoulos et al. (1999) found that the plasma flows in the plasma sheet are intermittent in nature. The magnetic field turbulence has been also studied. Using multispacecraft observations from Cluster, Weygand et al. (2005) were able to estimate turbulent eddy scale sizes in association with magnetic field fluctuations in the plasma sheet. Voros et al. (2004) introduced a wavelet technique to study magnetic turbulence, as obtained from the same Cluster satellite observations. In the work by Shiokawa et al. (2005), the power spectral indices were determined for magnetic fluctuations during nearEarth tail dipolarizations. The determination was done for the magnetic field magnitude fluctuations in the frequency range from 0.01 Hz to ~10 Hz, and the results show a steeper slope at a higher frequency regime.
Our goal in this study is to determine the degree of the anisotropic nature of the magnetic turbulence associated with magnetic dipolarizations in the plasma sheet. This has not been reported in any of the previous works on the Earth’s magnetospheric physics. For this study, we identified a total of 47 dipolarization events in a one month period, February 2008, using the magnetic field observations by the three neartail satellites, THEMIS A, D and E, when they were situated close to the neutral sheet. For the 47 events, we performed fast Fourier transform (FFT) power spectral analysis to estimate the spectral indices in the frequency regime from 1.3 mHz to 42 mHz, and compared them to determine the extent to which they can be anisotropic in a statistical sense.
2. METHOD AND EXAMPLE EVENT
First, we identified magnetic dipolarization events by using the magnetic field data provided at spin time resolution of 3 seconds, from the three THEMIS spacecraft,A, D and E, when they were at neartail, X ~ 7 to 12 R
_{E}
. To ensure close proximity of the satellites to the neutral sheet, we required that the average Bx to Bz ratio be less than 1 around the dipolarization onset time. For this study, a welldefined dipolarization was based on the requirement that Bz increase by 3 nT or more, or that the magnetic elevation angle increase by 10 deg or larger within 10 minutes after onset. However, since these simple criteria could lead to a false dipolarization, we checked all of the identified dipolarizations visually to determine whether they actually looked like a typical substormassociated dipolarization. Based on this set of criteria, we identified a total of 47 events in February 2008.
In this paper, we define a local coordinate system in which the three components of the magnetic field are decomposed into the parallel component, δB
_{II}
, and the two perpendicular components, δB
_{φ}
and δB
_{ψ}
, with respect to the background magnetic field. Here, the φ component refers to the azimuthal direction in the usual spherical coordinate system, and the ψ component completes the righthanded orthogonal coordinate system. The ψ coordinate refers to the poloidal flux coordinate. The use of the two perpendicular components, δB
_{φ}
and δB
_{ψ}
, can be useful in terms of understanding the polarization on the perpendicular plane, which can give a hint to the mode structure of instability during the fluctuations. Also, “δ” refers to the detrended values, which were obtained by applying a 5
^{th}
order polynomial fitting to the original data to obtain a trend (which is taken as a background field). We have calculated the spectral power densities based on the typical FFT method for the three components, δB
_{II}
, δB
_{φ}
and δB
_{ψ}
, for the 47 events. From this, we have determined the power spectral indices, α, for the three components, by applying leastsquare fits to the power spectral densities in loglog space, which are assumed to be of a form f
^{α}
, in which f refers to frequency.
Fig. 1
shows the magnetic field data (left) and the corresponding power spectral density (right) for an example event obtained from the THEMIS E observations on February 25, 2008. The original x, y, and z components, as well as the detrended components, δB
_{II}
, δB
_{φ}
and δB
_{ψ}
, of the magnetic field, are shown in the left panels. The power spectra were obtained by applying FFT to the 40 min time interval shown in the left panels (10 minutes before and 30 minutes after the dipolarization onset, as marked by the vertical line). From the power spectral curves, the spectral indices α for each magnetic component were estimated. In doing this, we have limited the fitting to the frequency range, 1.3 mHz up to 42 mHz (More discussion on this point is given in the last section). The values of α
_{II}
, α
_{φ}
and α
_{ψ}
for δB
_{II}
, δB
_{φ}
and δB
_{ψ}
are 0.74, 1.67, and 1.81, respectively, as indicated in the right panels, and thus, α
_{ψ}
> α
_{φ}
> α
_{II}
. This is an indication of the anisotropic spectral behavior of the magnetic turbulence.
3. STATISTICAL RESULTS
We performed a similar analysis for all of the 47 dipolarization events in the same manner as described above, and obtained the spectral power profiles and the associated spectral indices. The statistical results are analyzed in two different ways, as presented in
Figs. 2

4
. First,
Fig. 2
shows the scatter plots of the spectral indices α for all of the 47 events. The indices are presented for three pairs of two different components, so that a degree of anisotmulti
The magnetic field data (left) for a time interval on February 25 2008 observed by the THEMIS E spacecraft at X ~ 9R_{E} and the power spectra for the three detrended components (right).
Scatter plots of the spectral indices for the 47 dipolarization events as shown by comparing between a pair of two components.
Statistics of anisotropy between spectral indices.
ropy can be judged by visual observation. Note that a diagonal line is drawn in each panel to refer to the line of the isotropic values for a given pair of the indices; if the indices for the pair are the same for all of the 47 events, they should all lie on the diagonal line. For all of the three pairs, however, there are events off this line, implying some degree of anisotropy. For the pair α
_{φ}
and α
_{II}
, which is shown in the left panel, there is a slightly higher number of events (26 events) showing α
_{φ}
> α
_{II}
, than the opposite case (21 events). The middle panel shows that ~68% (32 events) of the 47 events are associated with a larger α
_{ψ}
than α
_{II}
. For the pair between α
_{ψ}
and α
_{φ}
(right panel), ~70% (33 events) of the 47 events are associated with a larger α
_{ψ}
than α
_{φ}
. When averaged over all 47 events, the spectral indices are <α
_{II}
>= 1.19, <α
_{φ}
> = 1.21, and <α
_{ψ}
> = 1.38, with standard deviations of 0.3, 0.4, and 0.4, respectively, implying a larger spectral index for the perpendicular directions than for the parallel direction in the statistical sense.
Fig. 3
shows the statistics for the ratios of the spectral indices for the perpendicular components to those for the parallel component. The degree of anisotropy ranges from ~0.2 to ~2.6, and the peaks of the ratios lie in the bin from 1 to 1.4.
Second, we have superposed the power density profiles of all of the 47 events to obtain average patterns, and this was done separately for each of the three detrended components, the results of which are shown in
Fig. 4
(left).
A visual inspection immediately indicates an overall
The superposed results of the power spectral profiles (left) and the corresponding linear fits done separately for two frequency domains shown in the separate panel for visual clarification (right) for the 47 dipolarization events.
steeper slope for the ψ component than for the other two, being basically consistent with the conclusion drawn in
Fig. 2
. Another interesting feature is that for all three components, there is a break frequency near ~0.008 Hz that divides the power profiles into two frequency domains having different slopes. By applying the linear fits to the two domains separately, the spectral indices were obtained, as indicated in the right panel. The spectral indices are largest for the ψ component in both domains. For reference, these are 1.08, 1.11, and 1.47 for α
_{II}
, α
_{φ}
and α
_{ψ}
, respectively, when the fits are done for the entire frequency domain without the division. Thus the largest index value, which is for the ψ component, is larger by >30% than that for the parallel component.
4. SUMMARY AND DISCUSSION
In summary, this paper reports on the determination of power spectral indices for the magnetic field fluctuations associated with magnetic field dipolarizations. For the study, we used the magnetic field data of the THEMIS A, D and E satellites in the neartail region, identified a total of 47 dipolarization events in February 2008, and performed the FFT power spectral analysis to estimate the spectral indices in the frequency regime from 1.3 mHz to 42 mHz. The obtained values of the indices clearly indicate the existence of anisotropic magnetic turbulence for many events. The degree of the anisotropy as defined by the ratios of the index of the perpendicular components to that of the parallel component can range from ~0.2 to 2.6. There are more events associated with a ratio larger than unity (i.e., the perpendicular index being larger than the parallel index) than those that are anisotropic in the opposite sense. Statistically, the spectral index for the perpendicular direction can be larger by >30% than that for the parallel direction. Also, it is more often the case that the ψ component index is larger than the φ component index in the perpendicular plane.
Our results are preliminary in a few aspects. The most serious defect is our choice of the frequency range, 1.3 mHz to 42 mHz, to apply linear fits. This is similar to what was used in Borovsky et al. (1997). The choice of such a frequency range has something to do with the concept of the socalled inertial range, for which the turbulence structure evolves in a conservative way. The inertial range is bounded by an injection frequency at which turbulence is initially excited, and a dissipation frequency at which the turbulence energy starts to dissipate. However, in the plasma sheet, it is largely unclear at the present time how (and if) one can define an inertial range. Clearly, further indepth research on this issue is required. For our preliminary study, we have selected this particular frequency range based on the following argument. The injection frequency is taken by assuming that the magnetic turbulence is driven by an excitation on a time scale of 1015 minutes. This is based on the currently popular view that magnetic dipolarizations are likely caused by the arrival of fast flows, having a time scale of 1015 minutes in many cases. The dissipation frequency is set by considering proton gyrofrequency in a magnetic field of 2530 nT. It has frequently been postulated that some kinetic dissipation process likely takes place on a time scale of ion gyrofrequency. Depending on the specific inertial range for which one does fitting to the power spectrum profiles, the spectral index values may differ from what we obtained. Nevertheless, we expect that the main point indicating the ψ?oriented anisotropy will remain valid, though further studies will have to test this when the concept of the inertial range is firmly settled.
Making a direct comparison of the present results with the usual magnetohydrodynamic (MHD) turbulence is not straightforward. One main reason for this is that one needs to convert the frequency spectra into the wave number spectra, and the best approach to this is still unclear. According to Borovsky et al. (1997) and Borovsky & Funsten (2003), a sweeping technique may be used under the Taylor hypothesis to obtain the implication that the spectral indices for the frequency spectra is preserved for the wave number spectra. However, the validity of this argument is not clear for the situations we have dealt with here. Nevertheless, if one is willing to accept the implication based on the argument by Borovsky et al. (1997) and Borovsky & Funsten (2003), a comparison of our results with the standard MHD turbulence theories can be done, as follows.
The homogeneous MHD turbulence theory suggests that the energy spectrum perpendicular to the local magnetic field direction is basically equivalent to the usual Kolmogorov spectrum, the spectral index being given by 5/3, and the parallel spectrum given by the larger spectral index value, 5/2. In contrast, our results indicate that the spectral indices for the perpendicular (parallel) components are often (always) smaller than the homogeneous MHD values. Furthermore, the characteristic anisotropy in the plasma sheet is quite different from, and is statistically opposite to, what the classic homogeneous MHD turbulence predicts. The precise reason for these differences is not currently understood, but they clearly imply that the nature of the turbulence of the usually inhomogeneous plasma sheet can differ significantly from the classic homogeneous MHD turbulence. A larger spectral index for the perpendicular fluctuations than for the parallel fluctuations implies that the fluctuation power decays toward the high frequency regime at a faster rate for the perpendicular fluctuations than for the parallel fluctuations. This could be related to a kinetic mechanism that causes the wave to decay more efficiently at the higher frequency in the plasma sheet. Observational test of this possibility may be worthwhile. We plan to further investigate these issues in the near future.
Acknowledgements
This work was supported by the research grant of Chungbuk National University in 2010. We are grateful to V. Angelopoulos, K. H. Glassmeier, U. Auster, W. Baumjohann and other THEMIS team members for the use of the THEMIS FGM data.
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Angelopoulos V
,
Mukai T
,
Kokubun S
1999
Evidence for intermittency in Earth’s plasma sheet and implications for selforganized criticality
PhPl
6
4161 
4168
DOI : 10.1063/1.873681
Borovsky JE
,
Elphic RC
,
Funsten HO
,
Thomsen MF
1997
The Earth’s plasma sheet as a laboratory for flow turbulence in high[beta] MHD
JPlPh
57
1 
34
DOI : 10.1017/S0022377896005259
Borovsky JE
,
Funsten HO
2003
MHD turbulence in the Earth’s plasma sheet: dynamics dissipation and driving
JGR
108
(A7)
1284 
DOI : 10.1029/2002JA009625
Park MY
,
Lee DY
,
Ohtani S
,
Kim KC
2010
Statistical characteristics and significance of lowfrequency instability associated with magnetic dipolarizations in the nearEarth plasma sheet
JGR
115
A11203 
DOI : 10.1029/2010JA015566
Shiokawa K
,
Shinohara I
,
Mukai T
,
Hayakawa H
,
Cheng CZ
2005
Magnetic field fluctuations during substormassociated dipolarizations in the nightside plasma sheet around X = ?10 RE
JGR
110
A05212 
DOI : 10.1029/2004JA010378
Voros Z
,
Baumjohann W
,
Nakamura R
,
Runov A
,
Volwerk M
,
Zhang TL
,
Balogh A
2004
Wavelet analysis of magnetic turbulence in the Earth’s plasma sheet
PhPl
11
1333 
1338
DOI : 10.1063/1.1667499
Weygand J
,
Kivelson MG
,
Khurana KK
,
Schwarzl HK
,
Thompson SM
,
McPherron RL
,
Balogh A
,
Kistler LM
,
Goldstein ML
,
Borovsky J
,
Roberts DA
2005
Plasma sheet turbulence observed by Cluster II
JGR
110
A01205 
DOI : 10.1029/2004JA010581