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**Annales Geophysicae**
An interactive open-access journal of the European Geosciences Union

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**Regular paper**
19 Sep 2019

**Regular paper** | 19 Sep 2019

Scaling laws in Hall inertial-range turbulence

^{1}Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, 8042 Graz, Austria^{2}International Space Science Institute, Hallerstrasse 6, 3012 Bern, Switzerland^{3}Geophysics Department, Ludwig-Maximilians-Universität, Theresienstraße 41, 80333 Munich, Germany

^{1}Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, 8042 Graz, Austria^{2}International Space Science Institute, Hallerstrasse 6, 3012 Bern, Switzerland^{3}Geophysics Department, Ludwig-Maximilians-Universität, Theresienstraße 41, 80333 Munich, Germany

**Correspondence**: Yasuhito Narita (yasuhito.narita@oeaw.ac.at)

**Correspondence**: Yasuhito Narita (yasuhito.narita@oeaw.ac.at)

Abstract

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There is an increasing amount of observational evidence in space plasmas for the breakdown of inertial-range spectra of magnetohydrodynamic (MHD) turbulence on spatial scales smaller than the ion-inertial length. Magnetic energy spectra often exhibit a steepening, which is reminiscent of dissipation of turbulence energy, for example in wave–particle interactions. Electric energy spectra, on the other hand, tend to be flatter than those of MHD turbulence, which is indicative of a dispersive process converting magnetic into electric energy in electromagnetic wave excitation. Here we develop a model of the scaling laws and the power spectra for the Hall inertial range in plasma turbulence. In the present paper we consider a two-dimensional geometry with no wave vector component parallel to the magnetic field as is appropriate in Hall MHD. A phenomenological approach is taken. The Hall electric field attains an electrostatic component when the wave vectors are perpendicular to the mean magnetic field. The power spectra of Hall turbulence are steep for the magnetic field with a slope of $-\mathrm{7}/\mathrm{3}$ for compressible magnetic turbulence; they are flatter for the Hall electric field with a slope of $-\mathrm{1}/\mathrm{3}$. Our model for the Hall turbulence gives a possible explanation for the steepening of the magnetic energy spectra in the solar wind as an indication of neither the dissipation range nor the dispersive range but as the Hall inertial range. Our model also reproduces the shape of energy spectra in Kelvin–Helmholtz turbulence observed at the Earth's magnetopause.

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Narita, Y., Baumjohann, W., and Treumann, R. A.: Scaling laws in Hall inertial-range turbulence, Ann. Geophys., 37, 825–834, https://doi.org/10.5194/angeo-37-825-2019, 2019.

1 Introduction

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The recent availability of multi-spacecraft missions
such as Cluster (Escoubet et al., 2001), THEMIS (Angelopoulos, 2008),
and MMS (Burch et al., 2016)
together with substantial advances in their instrumentation
and the subsequent data analysis opened up the door to a more detailed
study of space plasma turbulence on ion scales when ion inertia comes into
play. On those scales ions demagnetize and ultimately decouple magnetically
from the electron motion. The dropout of ions from magnetic dynamics
necessarily leaves its signature in the turbulent power spectra,
possibly causing deviations from the conventionally accepted
inertial-range slopes of turbulence.
Typical ion-inertial-range scale lengths in the solar wind range from
100 to 1000 km, which correspond to the turbulent wavenumber interval
${\mathrm{10}}^{-\mathrm{6}}\phantom{\rule{0.125em}{0ex}}\mathit{\lesssim}\phantom{\rule{0.125em}{0ex}}(\mathrm{2}\mathit{\pi}{)}^{-\mathrm{1}}k\phantom{\rule{0.125em}{0ex}}\mathit{\lesssim}\phantom{\rule{0.125em}{0ex}}{\mathrm{10}}^{-\mathrm{5}}$ m^{−1}. Multiplying, for instance,
with a nominal solar wind speed of ∼500 km s^{−1}
this interval maps to the frequency range
0.5 *≲* (2*π*)^{−1}*ω* *≲* 5 Hz.

Physically speaking, in a medium of density *n* moving at velocity ** V** the main
signature of the ion-inertial range,
sometimes also called the ion-kinetic regime or ion-dissipation range,
is the presence of Hall currents. These are pure electron currents
${\mathit{j}}_{\mathrm{H}}=-en\phantom{\rule{0.125em}{0ex}}\mathit{E}\times \mathit{B}/{B}^{\mathrm{2}}$ flowing
perpendicular to the magnetic

This ion-scale Hall turbulence is, for example in the solar wind,
two-dimensional with both wave vectors and fluctuating magnetic fields
confined to the plane perpendicular with respect to
the mean field *B*_{0}. Ion-kinetic-scale power-law spectra
(though limited to the frequency domain)
were observationally obtained separately
for the magnetic (Alexandrova et al., 2009; Sahraoui et al., 2009)
and electric (Bale et al., 2005) fields. They were found to be
reminiscent of a turbulent inertial range typical for scale-invariant
turbulence spectra of Richardson–Kolmogorov or Iroshnikov–Kraichnan type.

Dispersion analyses performed on the fluctuations showed the absence of any clear spectral eigenmodes (in linear Vlasov theory) which would result from dispersion relations in the presumable ion-scale wavenumber-frequency domain. At the best, there were rather weak indications found only of otherwise expected kinetic Alfvén, whistler, and ion Bernstein modes (Perschke et al., 2015, 2016; Roberts et al., 2015) in this range. The breakdown of linear-mode theory thus indicates that the frequencies deviate from simple Doppler-shifted linear modes by random sweeping which would be due to the large-scale variations of the flow such as eddies or Alfvénic fluctuations, sideband formation caused in both, a weakly turbulent kinetic wave–wave coupling, or steepening in the course of nonlinear evolution. Also solitary-structure formation resulting from phase coherence (Narita, 2018) seems to be absent. The study by Roberts et al. (2018) indicates the existence of the kinetic Alfvén mode in the magnetosheath region as obtained from the wave analysis for the fluctuations in the MMS data using the Alfvén ratio. No dispersion analysis is performed. On the other hand, the study by Narita et al. (2016) exhibits a frequency scattering in the observationally determined dispersion relation with an indication of a kinetic-drift mirror mode.

Based on these observations, we consider in the following a phenomenological turbulence model of stationary inertial-range spectra evolving in ion-scale turbulence. We will show that, qualitatively, such a model reproduces ion-inertial-range spectra measured by the MMS spacecraft in the vicinity of the magnetopause (Stawarz et al., 2016), whenever the Kelvin–Helmholtz instability is excited and decays into smaller-scale Kelvin–Helmholtz vortices until a spectrum of low-frequency small-scale turbulence is produced. We consider a two-dimensional geometry which has no parallel wave vector component. The full expression for the Hall electric field contains also parallel wave vector components (Treumann et al., 2019) which in Hall MHD are neglected.

Limitations of Hall MHD have been discussed, for example, by Howes (2009). The concept of Hall turbulence is valid in the limit where the electron temperature is much greater than the ion temperature and when the inverse of the linear transit time for an ion is much smaller than the turbulent frequency and the inverse of the linear transit time for an electron, respectively. Thus, in the instance where the temperature of the ions is finite, phase-mixing and damping of modes ought to be taken into account. This causes deviations from Hall MHD.

The results of our endeavor can be summarized as follows:
The Hall electric field attains the electrostatic
component when the wave vectors are perpendicular
to the mean magnetic field.
Scaling laws are derived for the magnetic field
and electric field in a power-law form.
In the case of the compressible magnetic field fluctuations
(with the parallel fluctuations of the magnetic field),
the energy spectra have a slope of $-\mathrm{7}/\mathrm{3}$ and $-\mathrm{1}/\mathrm{3}$
for the magnetic field and the Hall electric field, respectively.
The amplitude ratio of the Hall electric field to
the fluctuating magnetic field (hereafter, the ** E**–

2 The Hall fluctuation fields

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Separation of ion and electron motion in a streaming magnetized plasma generates
a Hall current *j*_{H}. Referring to the magnetized electron
equation of motion, which is the
generalized collisionless Ohm's law for the electric field, the Hall current produces
its specific Hall electric field:

$$\begin{array}{}\text{(1)}& {\mathit{E}}_{\mathrm{H}}=-{\displaystyle \frac{\mathrm{1}}{en}}{\mathit{j}}_{\mathrm{H}}\times \mathit{B}.\end{array}$$

The Hall current *j*_{H} is perpendicular to the magnetic and electric fields.
In turbulence theory one is interested in the fluctuations of the fields given
in the form $\mathit{\delta}\mathit{F}=\mathit{F}-{\mathit{F}}_{\mathrm{0}}$,
with ** F** referring to any relevant turbulent field,
magnetic, electric, flow velocity, density, and so on,
denoting fluctuations with prefix

$$\begin{array}{}\text{(2)}& \mathit{\delta}{\mathit{j}}_{\mathrm{H}}=-e\mathit{\delta}[n{\displaystyle \frac{\mathit{E}\times \mathit{B}}{{B}^{\mathrm{2}}}}{]}_{\mathrm{H}}\simeq -en{\displaystyle \frac{\mathit{\delta}{\mathit{E}}_{\mathrm{H}}}{B}}\times {\displaystyle \frac{\mathit{B}}{B}}.\end{array}$$

Electric field variations
contribute primarily to the linear Hall current fluctuations,
with fluctuating density and magnetic field contributions
being of higher order. As expected the turbulent Hall current
lies in the plane perpendicular to the mean field ** B** and is perpendicular
to the fluctuation in the Hall electric field. In the stationary observer's frame
there would be a number of other terms which, however, disappear in the moving
frame, the case which we are interested in here. There would also be
higher-order Hall current terms when folding with the
1st-order magnetic and electric field fluctuations
which we neglect to lowest order here.

The magnetic field fluctuations *δ**B*_{H} in Hall turbulence
have two components: one compressive component
*δ**B*_{‖} parallel to the mean field ** B** and the other perpendicular component

$$\mathit{\delta}\mathit{B}=(\mathrm{0},\mathit{\delta}{B}_{\u27c2},\mathit{\delta}{B}_{\Vert}).$$

The fluctuation of the Hall electric field is given by

$$\begin{array}{}\text{(3)}& \mathit{\delta}{\mathit{E}}_{H}={\displaystyle \frac{\mathrm{1}}{en}}\mathit{\delta}{\mathit{j}}_{\mathrm{H}}\times \mathit{B}-{\displaystyle \frac{\mathit{\delta}n}{n}}\mathit{E}.\end{array}$$

The last term on the right containing the fluctuations in density
and their contribution to *δ**E*_{H} is important only in the
stationary frame where ** E**≠0.
Using Ampère's law ${\mathit{\mu}}_{\mathrm{0}}\mathit{\delta}\mathit{j}=\mathrm{\nabla}\times \mathit{\delta}\mathit{B}$
(from here on suppressing the index H on the fluctuations when
dealing exclusively with Hall fluctuations in Hall MHD) yields

$$\begin{array}{}\text{(4)}& \mathit{\delta}\mathit{E}={\displaystyle \frac{\mathrm{1}}{en{\mathit{\mu}}_{\mathrm{0}}}}\mathit{B}\times (\mathrm{\nabla}\times \mathit{\delta}\mathit{B}).\end{array}$$

It follows from Eq. (4)
that in both cases the Hall electric field is along the perpendicular Hall
wave vector, i.e., along *e*_{1}. This shows that the fluctuation part
of the Hall electric field is purely electrostatic, a property of which
we can make use below. Switching to the Fourier representation with
∇→*i*** k** we obtain

$$\begin{array}{}\text{(5)}& {\displaystyle}\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}={\displaystyle \frac{\mathrm{i}}{en{\mathit{\mu}}_{\mathrm{0}}}}{k}_{\u27c2}\mathit{\delta}{B}_{\Vert}B\text{(6)}& {\displaystyle}\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{i}\right)}={\displaystyle \frac{i}{en{\mathit{\mu}}_{\mathrm{0}}}}{k}_{\u27c2}|\mathit{\delta}{B}_{\u27c2}{|}^{\mathrm{2}}\end{array}$$

for the compressive *δ**E*^{(c)} and incompressible
*δ**E*^{(i)} components of the wavenumber-parallel
(i.e., longitudinal fluctuation sense)
electric field fluctuations, respectively.
This shows that the incompressible electric field is 2nd order
in the magnetic fluctuation and will in principle be small and negligible.
The ratio of the two components

$$\begin{array}{}\text{(7)}& {\displaystyle \frac{\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{i}\right)}}{\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}}}={\displaystyle \frac{|\mathit{\delta}{B}_{\u27c2}{|}^{\mathrm{2}}}{B\mathit{\delta}{B}_{\Vert}}}\end{array}$$

depends on the sign of the compressive component of
the magnetic field *δ**B*_{‖}. Since its right-hand side
only contains magnetic components, it can be used in spacecraft observations
to estimate the ratio on the left. With this information the dominant
turbulent Hall electric field is given by the compressive magnetic Hall field
component, and the phase speed of the compressive Hall fluctuations is found to be

$$\begin{array}{}\text{(8)}& {\displaystyle \frac{\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}}{\mathit{\delta}{B}_{\Vert}}}={\displaystyle \frac{i{k}_{\u27c2}B}{en{\mathit{\mu}}_{\mathrm{0}}}}=i{V}_{\mathrm{A}}{\displaystyle \frac{{k}_{\u27c2}c}{{\mathit{\omega}}_{i}}}\end{array}$$

with *V*_{A} the Alfvén speed and *ω*_{i} the ion plasma frequency.
Squaring this, we obtain

$$\begin{array}{}\text{(9)}& ({\displaystyle \frac{\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}}{{V}_{\mathrm{A}}\mathit{\delta}{B}_{\Vert}}}{)}^{\mathrm{2}}={\displaystyle \frac{{k}_{\u27c2}^{\mathrm{2}}{c}^{\mathrm{2}}}{{\mathit{\omega}}_{i}^{\mathrm{2}}}}.\end{array}$$

The right-hand side of this expression is the rudiment of either a very
low-frequency ion wave or ion whistler dispersion relation which for ion
waves can be written as ${k}_{\u27c2}^{\mathrm{2}}{c}^{\mathrm{2}}/{\mathit{\omega}}_{i}^{\mathrm{2}}={\mathit{\omega}}^{\mathrm{2}}/{\mathit{\omega}}_{i}^{\mathrm{2}}-\mathrm{1}$ and which is
reproduced for *ω*=0. Thus the compressive part of Hall turbulence
can be understood as the zero-frequency fluctuations of transverse ion waves

$$\begin{array}{}\text{(10)}& {\displaystyle \frac{{k}_{\u27c2}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{V}}_{\mathrm{A}}^{\mathrm{2}}}{{\mathrm{\Omega}}_{i}^{\mathrm{2}}}}=\mathrm{1}-{\displaystyle \frac{{\mathit{\omega}}^{\mathrm{2}}}{{\mathrm{\Omega}}_{i}^{\mathrm{2}}}}{\displaystyle \frac{{V}_{\mathrm{A}}^{\mathrm{2}}}{{U}^{\mathrm{2}}}}\end{array}$$

in the limit *ω*→0, where $U=\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}/\mathit{\delta}{B}_{\Vert}$ is the complex phase
speed, and ${\stackrel{\mathrm{\u0303}}{V}}_{\mathrm{A}}={V}_{\mathrm{A}}^{\mathrm{2}}/U$ is a modified Alfvén speed, which shows
that these waves are essentially ion whistlers or modified zero-frequency Alfvén waves. Resolving for the fictitious frequency *ω*
one obtains

$$\begin{array}{}\text{(11)}& {\displaystyle \frac{\mathit{\omega}}{{\mathrm{\Omega}}_{i}}}=\pm {\displaystyle \frac{U}{{V}_{\mathrm{A}}}}\sqrt{\mathrm{1}+{\displaystyle \frac{{k}_{\u27c2}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{V}}_{\mathrm{A}}^{\mathrm{2}}}{{\mathrm{\Omega}}_{i}^{\mathrm{2}}}}}\sim \pm i{\displaystyle \frac{{k}_{\u27c2}c}{{\mathit{\omega}}_{i}}}\mathit{\eta}\end{array}$$

as can be shown by using the above expressions for *U*. Here *η*≈0
is a very small number. Nevertheless it is seen that, in principle,
these waves would have linear dispersion $\mathit{\omega}\sim \phantom{\rule{0.125em}{0ex}}{k}_{\u27c2}$ if attaining
any however small frequency. In addition, they would be damped.

What concerns the incompressible part (Eq. 6), so its phase speed becomes
a function of the transverse magnetic Hall field *δ**B*_{⟂}.
We should note that the ratio of electric-to-magnetic fields is
widely used in spacecraft observations in various plasma domains
as an estimator of the plasma convective motion
and the phase speed of the electromagnetic
wave (Matsuoka et al., 1991; Bale et al., 2005; Eastwood et al., 2009).

Ions are non-magnetic. So, since the Hall field is electrostatic and the wavenumber and electric field are aligned, the ions respond to the presence of an electric Hall field via Poisson's equation to generate an electric-fluctuation-related density fluctuation:

$$\begin{array}{}\text{(12)}& {\displaystyle \frac{\mathit{\delta}n}{n}}={\displaystyle \frac{i{\mathit{\u03f5}}_{\mathrm{0}}}{en}}{k}_{\u27c2}\mathit{\delta}{E}_{\u27c2}^{\left(\mathrm{c}\right)}={k}_{\u27c2}^{\mathrm{2}}{\displaystyle \frac{{V}_{\mathrm{A}}^{\mathrm{2}}}{{\mathit{\omega}}_{i}^{\mathrm{2}}}}{\displaystyle \frac{\mathit{\delta}{B}_{\Vert}}{B}}.\end{array}$$

Here, only the compressive field component contributes because of
its linearity. It shows that the relative density fluctuations are
completely determined by the compressive Hall magnetic field fluctuations
*δ**B*_{‖}. This is an important conclusion as it shows that the turbulent
density spectrum caused by the Hall effect is proportional to the
turbulent compressive magnetic Hall spectrum whose wavenumber dependence
is raised by the power of ${k}_{\u27c2}^{\mathrm{4}}$, an effect which should become observable
in the density spectrum in the scale range where ion inertia becomes susceptible.
There the Hall modification of the density spectrum adds to the non-Hall
deformation of the density spectrum derived in our former publication (Treumann et al., 2019).
We will briefly return to this item below after having constructed
the power spectrum of the magnetic fluctuations in the Hall field case.

3 Ion-scale inertial-range spectra

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In order to proceed quantitatively, we need to construct wavenumber
scaling laws for the spectra of the various field fluctuations.
Subsequently we intend to determine the ratio *δ**E*∕*δ**B* as well as
the energy spectra in an attempt to obtain a scaled model of
the ion-inertial-scale field fluctuations as the necessary step to derive
the turbulent inertial-range power spectra of the fields on ion-inertial-scale lengths $\mathrm{1}\phantom{\rule{0.125em}{0ex}}\mathit{\lesssim}\phantom{\rule{0.125em}{0ex}}kc/{\mathit{\omega}}_{i}<kc/{\mathit{\omega}}_{e}$ (where *ω*_{e} denotes the
electron plasma frequency).

To this end we turn to the application of a phenomenological turbulence model (Biskamp et al., 1996) in two-dimensional electron magnetohydrodynamics which is appropriate in our case. We have already made use of two-fluid plasma theory above when referring to the presence of the Hall effect in the generalized Ohm's law. Let us introduce the following scaling

$$\begin{array}{}\text{(13)}& \mathit{\delta}B\propto {\mathrm{\ell}}^{{\mathit{\alpha}}_{m}}\propto {k}^{-{\mathit{\alpha}}_{m}}\end{array}$$

for the turbulent magnetic field. We, moreover, normalize all relevant
fields and scales to the Alfvén speed *V*_{A},
ion cyclotron frequency Ω_{i}, and mean magnetic field *B* as follows:

$$\begin{array}{}\text{(14)}& {\displaystyle}\mathit{\delta}B\to \mathit{\delta}\stackrel{\mathrm{\u0303}}{B}={\displaystyle \frac{\mathit{\delta}B}{B}}\text{(15)}& {\displaystyle}\mathit{\delta}V\to \stackrel{\mathrm{\u0303}}{v}={\displaystyle \frac{\mathit{\delta}V}{{V}_{\mathrm{A}}}}\text{(16)}& {\displaystyle}\mathit{\delta}E\to \mathit{\delta}\stackrel{\mathrm{\u0303}}{E}={\displaystyle \frac{\mathit{\delta}E}{{V}_{\mathrm{A}}B}}\text{(17)}& {\displaystyle}\mathit{\delta}n\to \mathit{\delta}\stackrel{\mathrm{\u0303}}{n}={\displaystyle \frac{\mathit{\delta}n}{n}}\text{(18)}& {\displaystyle}k\to \stackrel{\mathrm{\u0303}}{k}={\displaystyle \frac{k{V}_{\mathrm{A}}}{{\mathrm{\Omega}}_{i}}}.\end{array}$$

In the two-dimensional compressible turbulence configuration,
the electron flow velocity is confined to the plane
perpendicular to the mean magnetic field,
but the magnetic field fluctuation *B*_{‖} is compressible.
The effect of the Hall effect on the fluctuation spectrum
implies that the magnetic field becomes
increasingly extended and compressed
like an elastic spring. The flow velocity is determined by the gradient
of the stream function as
$\stackrel{\mathrm{\u0303}}{\mathit{v}}=({\mathit{e}}_{\Vert}\times \stackrel{\mathrm{\u0303}}{\mathrm{\nabla}})\phantom{\rule{0.125em}{0ex}}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}$,
with the parallel fluctuation component $\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}$ of the
magnetic field playing the role of a stream function.
The eddy interaction time in units of the ion gyro-period ${\mathrm{\Omega}}_{i}^{-\mathrm{1}}$ becomes

$$\begin{array}{}\text{(19)}& \stackrel{\mathrm{\u0303}}{\mathit{\tau}}\propto (\stackrel{\mathrm{\u0303}}{k}\stackrel{\mathrm{\u0303}}{v}{)}^{-\mathrm{1}}\propto {\stackrel{\mathrm{\u0303}}{k}}^{-\mathrm{2}}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}^{-\mathrm{1}}.\end{array}$$

For the energy transfer rate, which is assumed to be constant over the entire turbulent inertial range, we have

$$\begin{array}{}\text{(20)}& \stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}\propto {\displaystyle \frac{|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}{|}^{\mathrm{2}}}{\stackrel{\mathrm{\u0303}}{\mathit{\tau}}}}\propto |\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}{|}^{\mathrm{3}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{\mathrm{2}}.\end{array}$$

This leads to the magnetic field scaling

$$\begin{array}{}\text{(21)}& \mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}\sim {c}_{m}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{1}/\mathrm{3}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{2}/\mathrm{3}},\end{array}$$

where a proper scaling coefficient *c*_{m} has been introduced.
With these expressions, the magnetic energy spectrum becomes

$$\begin{array}{}\text{(22)}& {\mathcal{E}}_{\mathrm{mag}}={\displaystyle \frac{|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}{|}^{\mathrm{2}}}{\mathrm{\Delta}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}}}\sim {c}_{m}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{2}/\mathrm{3}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{7}/\mathrm{3}},\end{array}$$

where the wavenumber interval is scaled to the wavenumber itself as $\mathrm{\Delta}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}\sim {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}$, i.e., assuming an equidistant grid on the logarithmic scale. This ${k}^{-\mathrm{7}/\mathrm{3}}$ scaling of the magnetic energy spectrum is intriguing in view of the same scaling which had been obtained in numerical simulations for isotropic Hall magnetohydrodynamic (Hall MHD) turbulence (Hori and Miura, 2008), the exact case which underlies our endeavor.

The energy spectrum for the Hall electric field fluctuation follows from the relation $\mathit{\delta}\stackrel{\mathrm{\u0303}}{E}={\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}$ together with Eq. (21) as

$$\begin{array}{}\text{(23)}& {\mathcal{E}}_{\mathrm{elec}}={\displaystyle \frac{{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{\mathrm{2}}|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}^{\mathrm{2}}}{\mathrm{\Delta}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}}}\sim {c}_{m}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{2}/\mathrm{3}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{1}/\mathrm{3}}.\end{array}$$

These two expressions can be used to calculate the ratio *δ**E*^{(c)}∕*δ**B*
of the fluctuation amplitudes

$$\begin{array}{}\text{(24)}& \left|{\displaystyle \frac{\mathit{\delta}{\stackrel{\mathrm{\u0303}}{E}}^{\left(\mathrm{c}\right)}}{\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}}}\right|=\sqrt{{\displaystyle \frac{{\mathcal{E}}_{\mathrm{elec}}}{{\mathcal{E}}_{\mathrm{mag}}}}}\sim {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2},\end{array}$$

which scales as the first power of the normalized wavenumber, indicating that the normalized fluctuation phase speed $\stackrel{\mathrm{\u0303}}{U}$ referred to linear increases above with decreasing scale in the ion-inertial range. Thus, this dependence remains unchanged and is in fact confirmed by the model.

Since for the turbulent Hall velocity fluctuations we have $\stackrel{\mathrm{\u0303}}{v}=\mathit{\delta}\stackrel{\mathrm{\u0303}}{E}$,
the kinetic energy spectrum ℰ_{kin}
scales like the electric power spectrum:

$$\begin{array}{}\text{(25)}& {\mathcal{E}}_{\mathrm{kin}}={\mathcal{E}}_{\mathrm{elec}}.\end{array}$$

As expected, the electric fluctuation spectrum in the Hall effect maps the kinetic fluctuation spectrum.

Finally coming to the spectrum of density fluctuations, we invoke Eq. (12), which in its rescaled form reads

$$\begin{array}{}\text{(26)}& \mathit{\delta}\stackrel{\mathrm{\u0303}}{n}=i{\left({\displaystyle \frac{{V}_{\mathrm{A}}}{c}}\right)}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{E}}^{\left(\mathrm{c}\right)}.\end{array}$$

It yields the turbulent Hall density power spectrum as

$$\begin{array}{}\text{(27)}& {\mathcal{E}}_{\mathrm{dens}}={\displaystyle \frac{|\mathit{\delta}\stackrel{\mathrm{\u0303}}{n}{|}^{\mathrm{2}}}{\mathrm{\Delta}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}}}\sim {\left({\displaystyle \frac{{V}_{\mathrm{A}}}{c}}\right)}^{\mathrm{4}}{c}_{m}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{2}/\mathrm{3}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{\mathrm{5}/\mathrm{3}}.\end{array}$$

Most interestingly, this spectrum is of an *inverse* Kolmogorov type.
Because of the relation between the Hall fluctuations in density and electric–magnetic fields, one of course expects that the presence of the Hall
effect in the ion-inertial range affects the shape of the density power spectrum.
This is indeed the case. In the ion-inertial-scale range the Hall effect
seems to practically compensate for the general spectral Kolmogorov slope
of the density power spectrum, causing it to flatten substantially.
Scaling-wise speaking,
this is quite a strong effect, the degree of whose signature
in observed density power spectra does, however, depend on the various scaling
constants in the spectral contributions. One may, however, speculate that the
notoriously frequently observed ${\stackrel{\mathrm{\u0303}}{k}}^{-\mathrm{1}}$ slope in the density power spectra
in the solar wind around the presumable ion-inertial-scale range,
for example in Šafránková et al. (2015),
may result from the contribution of the Hall effect to the inertial-range
spectrum of ion-inertial-scale turbulence.

It is interesting to compare the density spectrum with ${k}_{\u27c2}^{\mathrm{5}/\mathrm{3}}$ for the Hall scaling (Eq. 27) with the Kolmogorov–Poisson density spectrum with the ${k}_{\u27c2}^{\mathrm{1}/\mathrm{3}}$ scaling obtained earlier (Treumann et al., 2019, Eq. 24) for non-Hall turbulence. The ratio of the two expressions is

$$\begin{array}{}\text{(28)}& {\displaystyle \frac{{\mathcal{E}}_{\mathrm{dens}}^{H}}{{\mathcal{E}}_{\mathrm{dens}}^{K}}}\sim {\left({\displaystyle \frac{{V}_{\mathrm{A}}}{c}}\right)}^{\mathrm{2}}{\displaystyle \frac{{c}_{m}^{\mathrm{2}}}{{c}_{K}}}{k}_{\u27c2}^{\mathrm{4}/\mathrm{3}}.\end{array}$$

It still depends on the unknown constant of proportionality *c*_{m}
which must be determined otherwise. However, the deformation of the spectral scaling
caused by the Hall turbulence is stronger than in the non-Hall case. Its contribution
might thus become important, even though numerically its contribution to the density variation
is smaller than that of the Kolmogorov–Poisson spectrum, because
*V*_{A}≪*c*. The difference in the spectral slopes of ${k}_{\u27c2}^{\mathrm{4}/\mathrm{3}}$ indicates that
the Hall density spectrum becomes increasingly more effective at larger wavenumbers.

The Hall magnetic energy spectrum is steeper than the Kolmogorov-type one with wavenumber ratio

$$\begin{array}{}\text{(29)}& {\displaystyle \frac{{\mathcal{E}}_{\mathrm{mag}}^{H}}{{\mathcal{E}}_{\mathrm{mag}}^{K}}}\sim {k}_{\u27c2}^{-\mathrm{2}/\mathrm{3}}.\end{array}$$

Finally, the ratio of the kinetic power spectra yields a flatter Hall kinetic energy spectrum than Kolmogorov:

$$\begin{array}{}\text{(30)}& {\displaystyle \frac{{\mathcal{E}}_{\mathrm{kin}}^{H}}{{\mathcal{E}}_{\mathrm{kin}}^{K}}}\sim {k}_{\u27c2}^{\mathrm{4}/\mathrm{3}}.\end{array}$$

In this section we briefly turn to the incompressible Hall spectra.
As we had already noted, they play a lesser role in Hall turbulence
for the quadratic dependence on the incompressible Hall magnetic field
fluctuation component *δ**B*_{⟂} which would enable us to neglect it completely.
However, for the sake of completeness we provide the corresponding
expressions here below.

The scaling law in incompressible magnetic field fluctuations
is determined by the estimate of the flow velocity
in the perpendicular plane for the ** E**×

$$\begin{array}{}\text{(31)}& \stackrel{\mathrm{\u0303}}{\mathit{\tau}}\propto {\displaystyle \frac{{\stackrel{\mathrm{\u0303}}{\mathrm{\ell}}}_{\u27c2}}{{\stackrel{\mathrm{\u0303}}{v}}_{\u27c2}}}\propto {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{2}}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}^{-\mathrm{2}}.\end{array}$$

The energy transfer rate, again assumed to be constant in the inertial range, is

$$\begin{array}{}\text{(32)}& \stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}\propto {\displaystyle \frac{|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}{|}^{\mathrm{2}}}{\stackrel{\mathrm{\u0303}}{\mathit{\tau}}}}\propto {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{\mathrm{2}}|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}{|}^{\mathrm{4}}.\end{array}$$

The scaling law for the magnetic field follows from Eq. (32) as

$$\begin{array}{}\text{(33)}& \mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}\sim {c}_{m}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{1}/\mathrm{4}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{1}/\mathrm{2}},\end{array}$$

and the magnetic energy spectrum reads

$$\begin{array}{}\text{(34)}& {\stackrel{\mathrm{\u0303}}{\mathcal{E}}}_{\mathrm{mag}}={\displaystyle \frac{|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}{|}^{\mathrm{2}}}{\mathrm{\Delta}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}}}\sim {c}_{\mathrm{m}}^{\mathrm{2}}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{1}/\mathrm{2}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{2}}.\end{array}$$

The energy spectrum for the Hall electric field and that for the kinetic energy have the same spectral forms because again ${\stackrel{\mathrm{\u0303}}{u}}_{\u27c2}=\mathit{\delta}\stackrel{\mathrm{\u0303}}{E}$, yielding

$$\begin{array}{}\text{(35)}& {\stackrel{\mathrm{\u0303}}{\mathcal{E}}}_{\mathrm{elec}}={\stackrel{\mathrm{\u0303}}{\mathcal{E}}}_{\mathrm{kin}}\sim {c}_{m}^{\mathrm{4}}\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{-\mathrm{1}}.\end{array}$$

The ratio *δ**E*^{(i)}∕*δ**B* follows as

$$\begin{array}{}\text{(36)}& \left|{\displaystyle \frac{\mathit{\delta}{\stackrel{\mathrm{\u0303}}{E}}^{\left(\mathrm{i}\right)}}{\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}}}\right|\sim {c}_{m}{\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}}^{\mathrm{1}/\mathrm{4}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}^{\mathrm{1}/\mathrm{2}}.\end{array}$$

Even though the magnetic fluctuation field is incompressible, the density varies because of the electrostatic nature of the Hall field. The density spectrum for the Hall electric field is

$$\begin{array}{}\text{(37)}& {\mathcal{E}}_{\mathrm{dens}}\sim {\left({\displaystyle \frac{{V}_{\mathrm{A}}}{c}}\right)}^{\mathrm{4}}{c}_{m}\stackrel{\mathrm{\u0303}}{\mathit{\u03f5}}{\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}.\end{array}$$

Compared to the compressible case it increases at a lesser power with decreasing scale though also acting to compensate for the Kolmogorov slope.

Note that purely two-dimensional turbulence,
in which the gradients, wave vectors, and
field fluctuations are confined to the perpendicular plane,
is rather improbable in electron magnetohydrodynamics (EMHD) because the
** E**×

Figure 1 shows the schematic shapes of the Hall field spectra
in the ion-inertial range for the two cases of compressible and
incompressible Hall turbulence. Their absolute contribution to
the observed turbulence depends on the proportionality factor *c*_{m}
which enters all above expressions. It is, however, seen that
the kinetic energy in the Hall range dominates
the magnetic energy. This is of course reasonable because the Hall effect
is the result of the turbulence in the flow velocity. The dominant
effect is provided by the compressive part of Hall turbulence.
The compressive Hall magnetic spectrum decays slightly more steeply than
the Kolmogorov spectrum. One therefore expects that observed magnetic
spectra in stationary Hall turbulence in the ion-inertial-scale range
will obey inertial-range spectral indices ${k}^{-\mathrm{7}/\mathrm{3}}$.
On the contrary, however, the Hall density power spectra should exhibit a spectral
increase in the ion-inertial-scale Hall range which is due to
the reaction of the density to the
Hall electric turbulence. Naturally this effect is
more strongly expressed in the compressible case.

Since the total turbulence spectra in the ion-inertial range are composed of the superposition of Hall and non-Hall contributions, it becomes fairly clear that the ion-inertial-range spectra must deviate quite strongly from the inertial-range spectra of hydrodynamic turbulence (Richardson–Kolmogorov) or that of hydromagnetic turbulence (Iroshnikov–Kraichnan).

4 Conclusion and discussions

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The present communication dealt exclusively with the effect of the generation of Hall current turbulence in collisionless stationary homogeneous and isotropic inertial-range magnetohydrodynamic turbulence on ion-inertial scales $\mathrm{1}\phantom{\rule{0.125em}{0ex}}\mathit{\lesssim}\phantom{\rule{0.125em}{0ex}}kc/{\mathit{\omega}}_{\mathrm{i}}<kc/{\mathit{\omega}}_{\mathrm{e}}$ where ion inertia takes over to determine the dynamics and ions de-magnetize. This magnetohydrodynamic range also refers to Hall magnetohydrodynamics or electron magnetohydrodynamics. We first discussed in detail the appearance and properties of the Hall effect under conditions of interest in turbulence. We then switched and referred to a phenomenological scaling model. We derived the wavenumber scalings of the turbulent fluctuations and turbulent power spectral densities under Hall conditions. These investigations refer to the stationary frame of turbulence.

The first interesting result of this endeavor was that in stationary homogeneous turbulence the Hall contribution can be separated into compressive and non-compressive parts. It turned out that the compressive contribution to Hall turbulence dominates as it is 1st order in the turbulent magnetic field perturbation the Hall effect introduces. It was also found that the compressive Hall turbulence corresponds to kind of a zero-frequency ion wave whose complex phase speed is given by the ratio of electric and magnetic fluctuations. This phase speed increases with shrinking scale across the ion-inertial range being linearly proportional to the turbulent wavenumber.

Knowing the relations between the turbulent field fluctuations under the conditions when the Hall effect has to be taken into account in collisionless stationary and homogeneous turbulence, we considered the turbulent inertial Hall state. Turning to a dimensional analysis we were able to obtain the relevant scaling laws for the power spectral densities with respect to wavenumber holding in inertial-range Hall turbulent power law spectra.

Transition to phenomenological electron magnetohydrodynamics enabled the construction of the Hall inertial-range turbulent scaling laws on ion-inertia scales, an important and to our knowledge new finding which possibly enables the identification of the ion-inertial range from observation of magnetic, kinetic, and density turbulent power law shapes. For instance, the Hall turbulence model qualitatively explains the Hall-range energy spectra of the Kelvin–Helmholtz-type turbulence at the magnetopause (Stawarz et al., 2016) in that (1) the (electron) flow velocity and the electric field exhibit the same spectral curve perpendicular to the mean magnetic field; and (2) the magnetic energy spectrum is markedly steeper than that of the kinetic energy and the electric field energy.

Compressive inertial-range Hall magnetic power spectra scale like $\sim {k}_{\u27c2}^{-\mathrm{7}/\mathrm{3}}$, steeper than Richardson–Kolmogorov and Iroshnikov–Kraichnan while being, in some cases, in agreement with numerical simulations. This suggests that observed gradually increasing slopes in turbulent magnetic power spectra and becoming steeper at shorter scales than Kolmogorov may indicate that Hall turbulence on those scales takes over, and that the inertial-range turbulence enters the ion-inertia scales. If this happens, no reference is required to any sophisticated kind of hidden dissipation mechanism. Rather, this changing slope is quite a clear indication of the ion-inertial scale coming into play, clearer than the recalculation of scales via Taylor's hypothesis.

While the presented model is qualitatively similar to previous observations in that the magnetic energy spectra become steeper in the kinetic range, observed slopes are often steeper than $-\mathrm{7}/\mathrm{3}$, for example, as in Stawarz et al. (2016), Chen and Boldyrev (2017), and Breuillard et al. (2018). It should be noted that the theory predicts the energy spectra in the wave vector domain and the observations often have access to the spectra in the frequency domain. Possible reasons for the difference in the spectral slope between the theory and the observations include the presence of dispersive waves and the non-Gaussian frequency broadening in the random sweeping effect.

The turbulent Hall electric power spectra directly map the turbulent velocity power spectra, the most important kinetic power spectra in any turbulence. Since these at short scales are very difficult to measure, the observation of Hall turbulence should give a direct clue to their identification.

Hall turbulence quite strongly affects the inertial-range turbulent density spectra on ion-inertial scales,
as recently suggested (Treumann et al., 2019).
Hall density power spectra increase in their most important compressive and thus
dominant section as ${k}_{\u27c2}^{+\mathrm{5}/\mathrm{3}}$, which is an inverse Kolmogorov increase!
They contribute to the earlier found deviation from
inertial-range slope.
Observations should distinguish its absolute
contribution. This cannot be determined from phenomenological scaling theory.
The obtained steep spectral increase, when overlaid on ordinary spectra, might
contribute to the occasionally observed and still mysterious *k*^{−1} spectral slopes.

The data-analysis-motivated model of Alexandrova et al. (2008)
introduces an ad hoc measure *α*
of the compression distinguishing between the incompressible
(*α*=0) and isotropic compressible ($\left|\mathit{\alpha}\right|=\mathrm{1}$) cases.
It maps the spectral slope of the magnetic field
energy from ${k}^{-\mathrm{7}/\mathrm{3}}$ in the incompressible case
to $(-\mathrm{7}+\mathrm{6}\mathit{\alpha})/\mathrm{3}$ in the compressible case. Our
physically motivated Hall MHD model differs
from that of Alexandrova et al. (2008) in that the slope $-\mathrm{7}/\mathrm{3}$
is obtained for the compressible field fluctuations.

The Hall electric field attains the electrostatic component when the wave vectors are perpendicular or nearly perpendicular to the magnetic field. This applies to both the compressible and incompressible cases of magnetic fluctuations. The energy spectrum of the Hall electric field has a flatter spectral slope than that of the magnetic field.

Care must be exercised when analyzing
electric field data and estimating the
phase speed by reference to the ** E**–

Some observations
(Stawarz et al., 2016; Chen and Boldyrev, 2017) indicate the dominance of
the perpendicular magnetic field component
in the kinetic range.
Our scaling laws are derived separately for the
parallel one. It predicts that the Hall electric field
associated with the parallel component of the magnetic field
should dominate the electric spectrum (Eqs. 5–7).
The magnetic energy spectrum can be dominated by
either parallel or perpendicular fluctuations. However note
that the scaling contains the undetermined numerical
constant *c*_{m}, which determines the absolute value.

The parallel fluctuating component dominates
if both compressive and incompressible fluctuations are excited
by the electron flow. The normalized perpendicular component of the
magnetic field is smaller than the parallel component according to
$\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}\sim |\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}{|}^{\mathrm{2}}$.
This follows from the electron flow velocity
${\stackrel{\mathrm{\u0303}}{v}}_{\u27c2}\sim {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\Vert}$
and the association to the perpendicular component
${\stackrel{\mathrm{\u0303}}{v}}_{\u27c2}\sim {\stackrel{\mathrm{\u0303}}{k}}_{\u27c2}|\mathit{\delta}{\stackrel{\mathrm{\u0303}}{B}}_{\u27c2}{|}^{\mathrm{2}}$.
In Hall MHD the flow velocity is ** E**×

The relative contribution between the parallel and perpendicular components of the magnetic field depends on the length scales. Using Eq. (21) and Eq. (33) yields

$$\begin{array}{}\text{(38)}& {\displaystyle \frac{\mathit{\delta}{B}_{\Vert}}{\mathit{\delta}{B}_{\u27c2}}}\propto {\stackrel{\mathrm{\u0303}}{k}}^{-\mathrm{1}/\mathrm{6}}.\end{array}$$

Therefore, the contribution of the parallel component of the magnetic field is reduced with increasing wavenumber.

The increasing sense of the smaller-scale (or higher-frequency) density spectrum is indeed found using the Spektr-R spacecraft data in the solar wind (Šafránková et al., 2013). Treumann et al. (2019) provide a theoretical explanation of the density spectrum bump using the convected fluid model which the present theory extends to the inclusion of Hall dynamics. In the magnetosheath, to date no such increase has been observed in the electron density spectrum based on the spacecraft data. Figure 3 in Breuillard et al. (2018) shows a flattening of the density spectrum at spacecraft-frame frequencies of 10 Hz or higher, but this flattening is more likely associated with the Poisson noise in the particle measurements, indicating that clean, proper density spectrum measurements will be an important future task in the observational study of the Hall domain physics. Chen and Boldyrev (2017, their Fig. 4, bottom panel) shows that the density has about the same fluctuation power as the magnetic field at lower frequencies, indicating similar density and magnetic spectral slopes, with density spectrum estimated for electrons and inert ions. Theoretically, information about the density spectrum can also be obtained making use of either the continuity equation or the quasi-static approximation (Cohen and Kulsrud, 1974; Narita and Hada, 2018).

Schekochihin et al. (2009) provide a detailed description of ion-scale turbulence for weakly collisional plasmas through in a gyro-kinetic treatment. Gyro-kinetic theory is a reduced anisotropic limit of Hall MHD with comparable results to that of the authors. However, the gyrokinetic theory, unlike Hall MHD, incorporates phase mixing due to Landau damping (not cyclotron resonance). In weak turbulence of energy-cascading kinetic Alfvén waves, gyro-kinetic theory predicts inertial-range energy spectra (in the perpendicular wavenumber domain) with spectral slopes ${k}_{\u27c2}^{-\mathrm{1}/\mathrm{3}}$ for the electric and ${k}_{\u27c2}^{-\mathrm{7}/\mathrm{3}}$ the magnetic fields, and spectral density slopes ${k}_{\u27c2}^{-\mathrm{7}/\mathrm{3}}$. These are identical to the compressive magnetic field fluctuations obtained here.

In summary, we believe that the detailed analysis of the particular properties of the Hall inertial-range turbulence contributes to the clarification of the behavior of the plasma and electromagnetic field on the ion-inertia scales ${k}_{\u27c2}c/{\mathit{\omega}}_{i}>\mathrm{1}$, length scales shorter than that for the fluid or magnetohydrodynamic picture of turbulence. The wavenumber scaling laws and the corresponding power spectra are derived for Hall turbulent magnetic, electric, velocity, and density field in the phenomenological approach. The Hall inertial range is of great interest for many reasons in the both observational and theoretical sense.

In the observational studies of space plasma turbulence, various spectral observations have been performed in the past two decades, and there is an increasing amount of evidence that the magnetic energy spectrum exhibits a dissipative sense (steeper sense) of the spectral curve. Occasionally, it has even been called the dissipation (or ion dissipation) range. Excitation of ion-kinetic electromagnetic waves (such as highly oblique whistler mode, kinetic Alfvén mode, and ion Bernstein mode) is another possible scenario (which leads to the notion of dispersive range instead of dissipation range). Our model for the Hall turbulence serves as a likely candidate to explain the steepening of the magnetic energy spectra neither as dissipation range nor as dispersive range but as Hall inertial range.

In the theoretical studies, clarification of the spectral shapes in the Hall inertial range should provide a useful background for the distinction among the inertial-range behavior and dissipation of turbulence. Our Hall turbulence model shows that the inertial range can have a transition from fluid scales (which is for MHD) to ion scales (which is for Hall MHD) in a dissipationless manner. The dissipation of turbulent fluctuations in collisionless plasmas remains poorly understood. The difference in the spectral shapes from Hall inertial range would be interpreted as a sign of the onset of dissipation.

Author contributions

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Author contributions.

All the authors worked equally on the idea development, calculation, and manuscript writing.

Competing interests

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Competing interests.

The authors declare that they have no conflict of interest.

Financial support

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Financial support.

This research has been supported by the Austrian Research Promotion Agency (FFG) (Austrian Space Applications Programme (ASAP, grant no. 853994)).

Review statement

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Review statement.

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

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Short summary

Scaling laws and energy spectra for the electric field, magnetic field, flow velocity, and density are theoretically derived for small-scale turbulence in space plasma on which the electrons behave as a fluid but the ions more as individual particles due to the difference in the mass (the Hall effect). Our theoretical model offers an explanation for the small-scale turbulence spectra measured in near-Earth space.

Scaling laws and energy spectra for the electric field, magnetic field, flow velocity, and...

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