- Article
- Open Access

# Ballooning modes and their stability in a near-Earth plasma

- N. G. Mazur
^{1}Email author, - E. N. Fedorov
^{1}and - V. A. Pilipenko
^{2}

**65**:8

https://doi.org/10.5047/eps.2012.07.006

© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB. 2012

**Received:**13 February 2012**Accepted:**22 July 2012**Published:**10 June 2013

## Abstract

As a possible trigger of the substorm onset, the ballooning instability has been often suggested. The ballooning disturbances in a finite-pressure plasma immersed into a curved magnetic field are described with the system of coupled equations for the Alfven and slow magnetosonic modes. The spectral properties of ballooning disturbances and instabilities can be characterized by the local dispersion equation. The basic system of equations can be reduced to the dispersion equation for the small-scale in transverse direction disturbances. From this relationship the dispersion, instability threshold, and stop-bands of the Alfvenic and slow magnetosonic modes have been determined. The field-aligned structure of unstable mode is described with the solution of the eigenvalue problem in the Voigt model. We have also analyzed in a cylindrical geometry an eigenvalue problem for the stability of ballooning disturbances with a finite scale along the plasma inhomogeneity. The account of a finite scale in the radial direction raises the instability threshold as compared with that in the WKB approximation.

## Key words

- Plasma instability
- substorm onset
- MHD waves

## 1. Introduction: Ballooning Instability of Near-Earth Plasma as a Substorm Trigger

The key dilemma of the physics of terrestrial space environment is related to the identification of the substorm onset mechanism: does it occur in the magnetotail owing to magnetic field reconnection, or in a closed field line region as a result of some still unidentified instability? Tamao and his colleagues were the first who suggested that the ballooning instability could be a possible trigger of the substorm explosive phase (Miura et al., 1989; Ohtani and Tamao, 1993). This instability can be imagined as a distortion of radial gradient of hot plasma pressure by locally outward expansion and inward intrusion due to the azimuthally oscillating mode. The analysis of satellite observational data led Roux et al. (1991) to the suggestion that an instability driven by the plasma pressure gradient is responsible for the field-aligned current generation during the substorm onset. Later the idea about the ballooning instability as an onset trigger has been extensively elaborated (e.g., Lee and Wolf, 1992; Cheng et al., 1994; Liu, 1997; Cheremnykh et al., 2004; Agapitov et al., 2007).

In realistic magnetosphere the mechanisms of the ballooning instability in the near-Earth tail and reconnection in a distant magnetotail are probably coupled. The computer experiments with advanced models of the magnetosphere showed that the substorm onset was caused by violation of the balance between the thermal plasma pressure and Ampere’s force, resulting into the plasma expulsion and field lines extension into the magnetotail (Raeder et al., 2010). As a result, decrease of the magnetic component normal to the current sheet destabilized the tearing instability and stimulated the magnetic field reconnection. Thus, though the main substorm power is released via the reconnection, the substorm onset trigger could be the ballooning instability. To understand better the physical mechanisms of the processes involved in the substorm development, the results of the numerical modeling and in-situ satellite observations are to be compared with simplified, but more explicit, theoretical models.

A theoretical approach to the study of the ballooning instability is based on a complicated system of coupled equations for the poloidal Alfven waves and slow magnetosonic (SMS) modes in a finite-pressure plasma, immersed in a curved magnetic field **B** (e.g., Southwood and Saunders, 1985; Walker, 1987; Hameiri et al., 1991; Klimushkin and Mager, 2008). Favorable conditions for the instability growth emerge at a steep plasma pressure drop held by curved field lines. Such a condition may occur before sub-storm onset on strongly extended field lines.

The easiest way to comprehend qualitatively the basic features of the unstable modes and instability condition is the analysis of the local dispersion equation. The dispersion equation, obtained using a local analysis of this system, is widely used for geophysical applications both for the examination of plasma stability, and for the description of spectral properties of ULF wave phenomena in the nighside auroral magnetosphere (Safargaleev and Maltsev, 1986; Ohtani and Tamao, 1993; Liu, 1997; Golovchanskaya and Kullen, 2005).

However, the exact form of the dispersion equation used by different authors happens to be somewhat different, and the obtained results differ, too. Thus, it is necessary to check the derivation of the dispersion equation from basic MHD equations and the transfer to various limiting cases, which will be done in this paper.

In order to evaluate a field-aligned scale of ballooning-unstable modes, we consider the eigenvalue problem in the self-consistent analytical model of magnetic field and finite-pressure plasma (Voigt, 1986). However, an estimation of the instability criterion in the local approximation for a particular magnetic shell has necessarily a qualitative character because of the WKB approximation in the radial direction used during the solution of relevant equations. In a realistic situation an unstable mode near a steep gradient of the plasma pressure has a finite scale across the magnetic shells, which cannot be described by the WKB approximation.

Therefore, in this paper we consider the global stability with the use of very simplified magnetic field geometry (a cylindrical field with constant curvature field lines), which has enabled us to obtain some analytical results.

## 2. MHD Plasma Equilibrium and Linearized Dynamic Equations

We consider a finite pressure plasma confined by a 2D curved magnetic field **B**(*x, z*) with a local curvature radius *R*_{
c
}. We introduce a local orthogonal basis, organized by the **B** field geometry: **e**_{3} = **B**/*B* is in field-aligned direction, and **e**_{1} = **e**_{2} × **e**_{3} corresponds to the radial direction across magnetic shell. Along **e**_{2} = **e**_{
y
} (*Y*-axis) the system is homogeneous.

_{ n }=

**e**

_{ n }∙ ∇. The inhomogeneities of plasma and magnetic field are characterized by 3 local parameters:

*κ*

*P*=

*P*

^{−1}∇

_{1}

*P*,

*κ*

_{ B }=

*B*−1∇

_{1}

*B*, and the field line curvature . The local equilibrium condition of plasma with scalar pressure

*P*(

*x, z*) can be written via these

*κ*-parameters as follows:Under equilibrium the plasma pressure

*P*(

*x, z*) is constant along a field line.

*i*

*ω*

*t*) the linearized MHD equations arewhere

*ρ*is unperturbed density,

*ξ*is the plasma displacement, and

**b**and

*p*are disturbed magnetic field and pressure. We exclude

**b**from the first equation (2) and proceed from the variables

*ξ*

_{3},

*p*to the new variables:

*u*= ∇ ∙

*ξ*and the normalized disturbance of the total pressure

*q*=

*μ*

_{0}

*B*

^{−2}(

*p*+

*Bb*

_{3}/

*μ*

_{0}). The variable u characterizes the plasma compression and is related to its field-aligned displacement by the relationship . As a result we get the linearized MHD equations, which coincide with equations for 2D case from (Cheng, 2002), but for different variables:Here the following notations have been introduced:

*V*

_{ a }=

*B*(

*μ*

_{0}

*ρ*)

^{−1/2}is the Alfven velocity, is the Alfven wave number,

*V*

_{ s }= (

*γ*

*P*/

*ρ*)

^{1/2}is the sound velocity, is the sound wave number, is the “cusp ” velocity, and . We introduce also the following operators:

The typical time scale of the substorm explosive phase (~1−2 min) is much less than the Alfven transit time along the extended field lines from the magnetotail to the ionosphere (~10 min). Therefore, influence of the ionospheric boundaries on the ballooning mode properties can be neglected, assuming that the growing disturbances are localized in the near-equatorial region of the nightside magne-tosphere. The influence of the ionospheric boundary conditions on the ballooning modes was considered in many papers (e.g., Cheremnykh and Parnowski, 2006).

### 2.1 Asymptotic theory of transverse small-scale disturbances

For small-scale in the transverse (across **B**) direction disturbances the linearized MHD equations of a finite pressure plasma can be simplified and reduced to a system of ordinary differential equations for coupled Alfven and SMS modes. General approach to the 3D case with account for the gravity and plasma rotation effects was outlined by Hameiri et al. (1991). Our analysis of 2D configuration is given in another form.

*ξ*,

*u*,

*q*) ∝ exp(

*ik*

_{1}

*x*

_{1}+

*ik*

_{2}

*x*

_{2}) of the system (2) for large transverse wave numbers may be searched in the form(similar for

*u*and

*q*) where

*ε*is a small parameter.

*ε*

^{−1}it follows that the azimuthal displacement component

*ξ*

_{2}and the perturbation of the total pressure

*q*are small values of the order of . Further, in the zero-th order of

*ε*the closed system of equations occursThe system (4) is a special case of the system (71) from (Hameiri et al., 1991). It can be re-written in the following form (Klimushkin, 1998)

The relationship between different disturbance components is given by formulas
, and
. Both Alfven and SMS modes convey the field-aligned current
. For the ballooning disturbances (*k*_{2} ≪ *k*_{1}) the component *b*_{2} → 0, hence
.

### 2.2 Local dispersion equation

*ik*

_{ǁ}

*x*

_{3}) all operators turn into numerical factors , and . The linear system of differential equations (4) now becomes an algebraic system. The dispersion equation is obtained by setting the determinant of this system to zero, namelywhere . Equation (6) is a quadratic in

*Ω*

^{2}with rootswhere

*H*=

*β*

*κ*

_{ c }[2

*γ*

*κ*

_{ c }−

*κ*

_{ P }(2 +

*γ*

*β*)/2] sin

^{2}α. The roots (7) are real for a real

*k*

_{ǁ}.

_{+}) mode, which transforms into an Alfven wave as

*β*→ 0, and slow (Ω

_{−}) mode. Their dispersion curves are shown in Fig. 1. The fast branch is stable for any

*k*

_{ǁ}. Only the slow mode can be unstable under the conditionThis inequality is the generalization for oblique disturbance with

*k*

_{1}≠ 0 of the ballooning instability condition (Liu, 1997). The maximal value of the growth rate as estimated from the dispersion relation (7) isIf

*κ*

*b*≪

*κ*

*c*, then, taking into account (1), (9) is reduced to .

*k*

_{ǁ}≫

*κ*

_{ c }sinα:where . Here the parameter Λ =

*κ*

_{ P }/

*κ*

_{ c }has been introduced. Its absolute value ǀ Λ ǀ =

*R*

_{ c }/

*a*is the ratio between the curvature radius

*R*

_{ c }and the plasma inhomogeneity scale . When Λ < 0 (outward pressure gradient) both branches are stable. When Λ > 0 (inward pressure gradient), the interval emerges according to (8), where , thus the slow mode branch turns out to be unstable.

### 2.3 The possibility of total reflection of poloidal Alfven waves

*Ω*there may occur regions where (see dispersion curves in Fig. 2). These regions are non-transparent (opaque) for poloidal Alfven waves. Their occurrence can be qualitatively shown with the use of the formula (7) for . Wave meets the turning points when its frequency

*Ω*matches the cut-off frequencyThe exact formula (12) differs somewhat from that in (Mager et al., 2009) obtained with the use of asymptotic relationship (11). In a disturbed nightside magne-tosphere with tailward extended field lines, the curvature ǀ

*κ*

_{ c }(

*x*

_{3})ǀ increases sharply equatorward, therefore, in the near-equatorial region the condition may be fulfilled, and becomes negative in this area. This region with high

*β*and locally curved field lines is non-transparent for poloidal Alfven waves.

## 3. Field-Aligned Structure of Unstable Modes

*P*and vector potential of the magnetic field

*A*=

*A*

_{ y }, namely

*P*= (2

*μ*

_{0})

^{−1}

*K*

^{2}

*A*

^{2}, where the parameter

*K*characterizes the magnetic field distortion by the plasma pressure. Thanks to this assumption the equilibrium Grad-Shafranov equations become linear, and the equation for the potential

*A*(

*x, z*) can be obtained. The solution of this equation in the band (which models a magnetosphere engulfed by the solar wind) with the dipole source in the coordinate origin has the form (at )where

*B*

_{ e }is the magnetic field at the Earth’s equator,

*R*

_{ e }is the Earth’s radius, , and . The function

*A*(

*x, z*) is constant along a field line. The background magnetic field and its transverse gradient are derived via

*A*(

*x, z*) as followsUsing the expressions (14) one can find the parameters which determine the coefficients of the system (4):

*β*=

*K*

^{2}

*A*

^{2}

*B*

^{−2},

*κ*

_{ P }= 2

*BA*

^{−1}, and . The form of a field line

*x*=

*x*(

*s*),

*z*=

*z*(

*s*) can be determined by the solution of the differential equations which depend on the parameter

*K*: when

*K*increases the field line becomes more extended. With the use of (13) and (14) distribution of the basic parameters along a field line can be determined.

*k*

_{2}≫

*k*

_{1}. The spectrum of eigenfrequencies comprises the infinite number of stable discrete modes and an unstable mode with . The field-aligned structure of the unstable eigenmode at

*L*= 10

*R*

_{ e }has been numerically modeled (Fig. 3). In a high-pressure plasma,

*β*

_{max}≃ 20, both the magnetic field compression

*b*

_{ǁ}and transversal plasma displacement

*ξ*

_{1}of the unstable disturbance are localized in vicinity of a field line top. The field-aligned scale of disturbance is about ±1.5

*R*

_{ e }, hence it is localized within the same region where

*β*is high.

## 4. Global MHD Stability of the Ballooning Mode in a Cylindrical Geometry

In contrast to the local analysis of the plasma stability in Section 2, here we perform a global analysis, but in the framework of a simple cylindrical model. The cylinder axis is along coordinate *y*, which corresponds to the azimuthal direction in the magnetosphere. Magnetic field lines are circles with radius *r*. This simplified model possesses all the typical features necessary for occurrence of the ballooning instability: field line curvature and a plasma pressure gradient. This model can be considered as an element of a more general configuration, specifically in the region of strongly disturbed field lines. The structure of the disturbance harmonic along a field line is assumed to be ∝ exp(− *i*ω*t* + *iv**θ*), where the parameter *v* determines the field-aligned wave number as *k*_{ǁ} = *v/r*.

*ξ*=

*ξ*

_{ r }and the normalized disturbance of the total pressure

*q*:The coefficients of this system are as follows:Here the operators have been reduced to the algebraic factors , and . Our consideration is not limited by the transversely small-scale limit

*k*

_{⊥}→ ∞, so the system (15) describes coupled Alfven, fast magnetosonic (FMS), and SMS modes for arbitrary transverse scales.

*a*is the typical scale of inhomogeinity, and

*r*

_{0}is the position of the plasma gradient maximum. The pressure drops to some background level far from the plasma gradient:

*P*→

*P*

_{∞}at

*r*→ ∞, whereas the density distribution

*ρ*(

*r*) is homogeneous. The parameter

*β*

_{0}=

*β*(

*r*

_{0}) varies within the limits 0–1, and characterizes the global “temperature ” of a plasma; its increase results in the raising of the

*β*(

*r*) profile. For values of

*β*

_{0}→ 1, the local values of the actual

*β*(

*r*) parameter may be rather high: max

*β*(

*r*) ~ 10 if

*β*

_{0}= 0.95 and

*a*/

*r*

_{0}= 0.1.

## 5. The Boundary Problem for the Growth Rate Determination

We consider the boundary problem for the system (15) in a semi-infinite interval with the boundary condition *ξ*(*R*_{
e
}) = 0 and the requirement of bounded *ξ* (*r* ) as *r* → ∞. The system parameters for which instability is possible are determined by the occurrence of discrete eigenvalues
. The values
, when this problem has a solution, determine the growth rates Γ = Im ω > 0 for the corresponding eigenfunctions.

*q*from (15) and using the standard change of variables technique one arrives atThe function

*I*(

*r*) plays the role of the squared local radial wave number , and is determined by a cumbersome combination of the coefficients (16) and their derivatives. A bounded solution may occur only when

*I*(

*r*) > 0 in a sufficiently long interval. An example of the

*I*(

*r*; ω

^{2}) dependence, when discrete spectrum can emerge, is shown in Fig. 4 (top panel). When the absolute magnitudes of negative ω

^{2}are large, the function

*I*(

*r*) < 0 for all

*r*> 0, hence a bounded solution does not exist. When ω

^{2}grows and approaches zero, an interval emerges where

*I*(

*r*) > 0, therefore the occurrence of discrete eigenvalues becomes possible. The eigenvalues of the boundary problem and the corresponding eigenfunctions have been calculated numerically. An example, when the spectrum comprises 3 eigenvalues, is presented in Fig. 4 (bottom panel).

*β*

_{0}. In the limit

*β*

_{0}→ 0 the spectrum evidently does not exist. For

*v*≠ 0 there is a threshold value of (v) for the plasma stability. For a higher

*β*

_{0}the growth rate further increases.

The dependence of eigenvalues
on the azimuthal wave number *k*_{
y
} for a given *v* = 0.5 is shown in Fig. 5 (right-hand panel). The model used enables us to consider the instability pattern for an arbitrary *k*_{
y
}. This consideration shows that the instability is possible even for azimuthally large-scale modes,
. The growth rate increases rapidly with the increase of *k*_{
y
} and at
gradually reaches the saturation.

*k*

_{ y }→ ∞ is as followsThe comparison of the instability thresholds in the WKB approximation (19) and obtained by numerical solution is given in Fig. 6. The solid line shows the extreme value of the destabilizing term -

*β*

*κ*

_{ P }

*r*for different azimuthal scales

*k*

_{ y }

*a*. The disturbances with

*v*

^{2}< max(-

*β*

*κ*

_{ P }

*r*) are unstable. The dashed lines show the critical value of

*v*, above which the discrete spectrum is absent. Thus, for any

*v*the threshold by parameter

*β*

_{0}for disturbances of finite-scale along the radius is higher than the threshold predicted by the local theory (19).

## 6. Discussion

The description of the ballooning instability by (Ohtani and Tamao, 1993) owing to a mathematical error (Liu, 1997) resulted in an incorrect conclusion about the possible instability of both wave branches. Miura et al. (1989) predicted a possible instability of Alfven-type disturbances with the growth rate
. However, their assumption *u* = 0 (or *ξ*_{ǁ} = 0) used for isolating the Alfven mode turns out to be inconsistent with the second equation from the basic system (4). Analysis of the dispersion relationship (6) in the poloidal limit *k*_{1} = 0 shows that no branch
can intersect the line
. The relation
from (Miura et al., 1989) contradicts this condition. Thus, the Alfven-type branch is always stable,
.

The favorable conditions for the balloon instability growth may occur under strongly extended into the magne-totail field line before the substorm onset (Zhu et al., 2009). At the linear stage of the ballooning instability a disturbance grows exponentially, though drift effects may produce oscillatory growth and azimuthal drift with the velocity of about the Larmor drift velocity (Miura et al., 1989).

Using the energy principle, the ideal MHD stability of ballooning-type perturbations for a “hard ” ionospheric boundary condition was considered by Lee and Wolf (1992). For self-consistent analytical model of the magnetosphere, they found that if a magnetotail configuration was stable to interchange, it was also stable against symmetric ballooning. We suppose that in a realistic magnetosphere the ballooning modes are to be localized near the mag-netospheric equator, where the parameter *β* and curvature rapidly increase. Indeed, the field-aligned structure of unstable ballooning modes described within the Voigt model is strongly localized in the vicinity of the top of field lines.

In a radial direction the growing disturbances are localized in the region of pressure gradient, whereas the scale of fundamental mode is about the pressure inhomogeneity scale. The radial fundamental mode has a lowest threshold in respect to the parameter *β*_{0}, whereas the threshold value *β*_{0} is higher than it follows from the local criterion. The az-imuthally small-scale disturbances with *k*_{
y
}*a* ≫ 1 have the growth rate of the fundamental mode Γ ≃ (*V*_{
A
}/*a*)ImΩ ≃ 0.03 c^{−1} for *V*_{
a
} = 500 km/s and *a* = 0.8*R*_{
e
}. This value agrees with the estimate following from the local approximation (9). The characteristic growth time of the instability ~ Γ^{−1} ≃ 30 s is about the typical time scale of the substorm explosive phase.

The cylindrical model has enabled us to consider the stability for an arbitrary *k*_{
y
}, which showed that even an azimu-tally large-scale mode, *k*_{
y
}*a* ≪ 1, can be destabilized. Such mode, named *KY0* mode, indeed was found unexpectedly during numerical modeling (Raeder et al., 2010). The instability growth rate increases with the increase of *k*_{
y
} in the range
, and reaches the saturation for the azimuthal wave numbers
. This behavior fits the results of the numerical modeling (Zhu et al., 2004).

For the considered model the source of free energy for the ballooning instability is the excess of the hot plasma pressure in the radial direction. However, our model does not take into account few factors which might be significant for the instability development: pressure anisotropy (Cheng and Qian, 1994), drift effect (Miura et al., 1989), kinetic effects (Klimushkin and Mager, 2008), and the azimuthal pressure gradient related to a background field-aligned current (Ivanov et al., 1992; Golovchanskaya and Maltsev, 2003). The ballooning instability can be excited nonlin-early by an external trigger (Hurricane et al., 1999). For such “MHD detonation ” the magnetospheric plasma must be near the threshold level, determined by the linear theory of instability, and an external trigger must have a magnitude sufficient to transfer the system into the nonlinear explosive growth phase.

## 7. Conclusion

We have discussed the dispersion relationship, instability threshold, and stop-bands for the Alfvenic-type and SMS-type modes which can be used for space applications. The Alfven-type branch is always stable. For poloidal Alfven waves with frequencies less than the cut-off frequency (12) a non-transparent region may occur, which makes the wave propagation along the whole field line impossible.

In the region with a steep drop of the finite pressure plasma, held by curved magnetic field lines, an instability of the SMS-type mode may become feasible. When the ballooning instability threshold is exceeded the hot plasma expands locally outward. The disturbance grows aperiodi-cally, though drift effects (neglected here) may produce an oscillatory growth. Unstable disturbance is strongly localized in the region of a field line with high *β* and strong curvature.

In the radial direction unstable disturbances are non-propagating modes localized near the plasma gradient. The fundamental mode has the lowest threshold, whereas the threshold per se is somewhat higher than what follows from the local criterion.

## Declarations

### Acknowledgments

This study is supported by grant 13-05-90436 from RFBR and Program 22 of Russian Academy of Sciences. We appreciate constructive suggestions of both reviewers.

## Authors’ Affiliations

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