Rotational properties of annulus dusty plasma in a strong magnetic field

The collective dynamics of an annulus dusty plasma formed between a co-centric conducting (non-conducting) disk and ring configuration is studied in a strongly magnetized radiofrequency (rf) discharge. A superconducting electromagnet is used to introduce a homogeneous magnetic field to the dusty plasma medium. In the absence of the magnetic field, the dust grains exhibit thermal motion around their equilibrium position. The dust grains start to rotate in the anticlockwise direction with increasing magnetic field (B > 0.02 T ), and the constant value of the angular frequency at various strengths of the magnetic field confirms the rigid body rotation. The angular frequency of dust grains linearly increases up to a threshold magnetic field (B > 0.6 T ) and after that its value remains nearly constant in a certain range of magnetic field. Further increase in magnetic field (B > 1 T ) lowers the angular frequency. Low value of the angular frequency is expected by reducing the width of the annulus dusty plasma or the input rf power. The azimuthal ion drag force due to the magnetic field is assumed to be the energy source which drives the rotational motion. The resultant radial electric field in the presence of a magnetic field determines the direction of rotation. The variation of floating (plasma) potential across the annular region at given magnetic field explains the rotational properties of the annulus dusty plasma in the presence of a magnetic field.     

A model of Jupiter’s magnetodisk

An axially symmetric equilibrium model of Jupiter’s magnetodisk is developed in the MHD approximation that takes the plasma corotation and the centrifugal force into account. The model is constructed for two cases: (1) the magnetodisk plasma is assumed to have a uniform temperature; (2) the plasma pressure is assumed to be an adiabatic function of density. Analytical expressions for the magnetic field, current density, and magnetodisk temperature and thickness distributions are obtained as functions of the system parameters, viz., the radial distribution of plasma pressure in the equatorial plane, the transverse magnetic field in the center of the layer, and the angular velocity of the plasma rotation.     

Propagation effects in the radio interferometry of polarized radiation: II. Fluctuations of polarized radiation in a random magnetoplasma

This paper analyses fourth-order moments of polarized radiation passing through magnetoactive plasma with random irregularities both in electron density and in magnetic field. We consider the new propagation effect arising from chiral properties of random magnetoplasma. That is, the lens formed by the same irregularities of magnetic field may be characterized by refractive properties of opposite sense vis-a-vis the rotation of the wave polarization vector. This produces an appearance of slight circular polarization fluctuations arising from initially nonpolarized radiation. Analysis of the polarized radiation fluctuations may allow the spatial spectrum of magnetic field irregularities to be detected. The enhanced level of the circularly polarized component, and the share of fluctuations owing to magnetic field irregularities, can be readily observed at low frequencies only, say, in the radiation passing through the solar chromosphere or the Jovian and terrestrial ionosphere, (magnetosphere).     

Energy Characteristics of Wave Fields Radiated from Elementary Oscillators in a Nondispersive Medium Moving with Subluminal Velocity

We study the energy characteristics of fields radiated from electric, magnetic, and toroidal dipoles in a nondispersive medium moving with velocity lower than the speed of light in this medium. The angular dependences of Abraham's energy-flux density of electromagnetic field are analyzed. In particular, it is shown that if the medium velocity is high enough, then the radial component of the vector of energy-flux density is negative in a certain angular range. Expressions for the electromagnetic energy flux through a sphere of large radius are obtained. It is shown that if the velocity of a moving medium is high enough, then the energy flux is negative and its absolute value can exceed the energy losses of sources.     

Satellite observations of electric fields in the innermagnetosphere and their effects in the mid-to-low latitude ionosphere

During geomagnetic disturbances, momentum and energy are transferred in significant quantities from interplanetary space to the magnetosphere-ionosphere system through the mediation of charged particles and electric fields. The most dramatic manifestations occur in the plasma sheet and the conjugate auroral ionosphere. However, electric fields observed during magnetic storms also penetrate the inner magnetosphere that maps to subauroral latitudes in the ionosphere. For example, a sudden commencement shock wave initiating the March 1991 magnetic storm created a new radiation belt within minutes. Particle and field measurements by Combined Release and Radiation Effects Satellite (CRRES) near the equatorial plane of the magnetosphere and by Defense Meteorological Satellite Program (DMSP) satellites in the topside ionosphere during the magnetic storm of June 1991 indicate that penetration electric fields energized the stormtime ring current and rapidly transported plasma within subauroral ion drift (SAID) structures at midlatitudes and in upward drafting plasma bubbles at low latitudes. Through enhanced transport or chemical reactions, the SAIDs dug deep plasma troughs at topside altitudes. Equatorial plasma bubbles developed while the ring current was unable to shield the electric field from the innermost magnetosphere     

Generation of Electric Fields and Currents in the Earth's Ionosphere Within the Framework of the Planetary-Generator Model

We present a solution for the problem of generation of electric fields and currents in the lower ionosphere of the Earth due to the nonuniform rotation of the magnetized planet and its plasma envelope with inhomogeneous conductivity (the planetary generator model). The angular velocity _p(r,) and the conductivity profile (r) of the plasma envelope are specified taking into account the experimental data. It is shown that under these conditions, the current system of the planetary generator is a single current loop localized mainly in a narrow layer corresponding to the high-conductivity region at heights h₁100 km. The thickness of this layer is about the conductivity scale. Within the framework of this model, we estimate the total current circulating in the ionosphere and the current flowing in the planet and calculate the characteristic values of the electric fields generated. Comparison between the calculation results and the experimental data shows that the considered mechanism of current generation can be significant for analyzing current systems in the lower ionosphere of the Earth.     

The solar wind interaction with the Earth's magnetosphere: atutorial

The size of the terrestrial magnetosphere is determined by the balance between the solar wind dynamic pressure and the pressure exerted by the magnetosphere, principally that of its magnetic field. The shape of the magnetosphere is additionally influenced by the drag of the solar wind, or tangential stress, on the magnetosphere. This drag is predominantly caused by the mechanism known as reconnection in which the magnetic field of the solar wind links with the magnetic field of the magnetosphere. The factors that control the rate of reconnection of the two fields are not understood completely, but a southward direction of the interplanetary field is critical to enabling reconnection with the dayside low-latitude magnetosphere, resulting in magnetic flux transfer to the magnetotail. Numerical simulations suggest that the conductivity of the ionosphere controls the rate of reconnection, but this has not been verified observationally. Although solar wind properties ultimately control the interaction, the properties of the plasma that make direct contact with the magnetosphere are different than those of the solar wind, having been altered by a standing bow shock wave. This standing shock is necessitated by the fact that the flow velocity of the solar wind far exceeds the velocity of the compressional wave that diverts the solar wind around the Earth. The upper atmosphere is the final recipient of all the energy and momentum that enters the magnetosphere. Coupling takes place along the magnetic field Lines principally in the polar and auroral region via current systems that close across the magnetic field both at low and high altitudes and flow parallel to the magnetic field between high and low altitudes     

Registering Jovian electrons in the Earth’s orbit

The results from observing Jovian electrons in the vicinity of the Earth are discussed. Variations in Jovian electron flows are observed during 14 rotations of the Sun in 2007–2008. The results are analyzed by assuming the existence of magnetic traps in the space between the Sun and Jupiter that are filled with electrons near Jupiter, and are then registered when the traps pass by the Earth. The average period of variation in the Jovian electron flow during the 14 solar rotations is 26.2 days instead of the expected synodic period of the Sun–Earth system equal to 27.3 days. An explanation for this phenomenon is proposed.     

On the structure of the middle Jovian magnetosphere

A model of the plasma distribution in the middle Jovian magnetosphere is considered. The distribution of the background plasma along the magnetic lines of force under the action of the centrifugal force and the force of gravity is analyzed in the framework of the diffusive equilibrium, taking into account the finite angle between the magnetic and rotational axes. It is shown that the dense structures of the background plasma have the form of a warped sheet located between the magnetic and centrifugal equators, and of two mirror symmetrical petals in the vicinity of the polar cusps. The hydrodynamic stability of the dense plasma sheet, formed under the action of the centrifugal force, is studied. The steady state radial plasma distribution at the threshold of the instability with respect to the small-scale MHD perturbations is determined. The finite conductivity of the Jovian ionosphere is taken into account. The influences of the longitudinal inhomogeneity of the perturbations, the finite ion Larmor radius, and the curvature of the magnetic field lines on the threshold of the instability are estimated. Some aspects of the formation of the energetic particle distribution in the middle Jovian magnetosphere are considered. The suggested model shows reliable agreement with the known experimental data and is also useful in describing the background plasma distribution in the magnetospheres of Neptune and Uranus.Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod. Traslated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 37, No. 5, pp. 580–595, May, 1994.     

On the fine structure of the Jovian decametric dynamic spectrum

A general concept of Jovian decametric radiation is proposed that allows various approaches to the problem of the origin of this radiation to be coordinated. The concept is used to explain the origin of such fine-structure characteristics of the dynamic spectrum as frequency splitting of the high-frequency part of the spectrum and the shape of the spectral arcs. The plasma density and velocity of radiating electrons in the force tube of the planet's magnetic field near the L-shells corresponding to Io.Institute of Applied Physics, Russian Academy of Sciences. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 37, No. 6, pp. 693–706, June, 1994.     

Effect of limiting polarization in the Jovian inner magnetosphere

Jovian decameter emission is known to exhibit almost total polarization. We consider the elliptical polarization to be a consequence of linear-mode coupling in the Jovian magnetosphere outside the source region. We determine conditions of emission propagation along the ray path that are necessary for self-consistent explanatation of the polarization observations and show that the ellipticity (axial ratio of the polarization ellipse) is determined by the magnetospheric plasma density n_e in a small region a distance of about half the Jovian radius from the radiation source. The plasma density in the region is quite low, n_e<0.4 cm⁻³, and the geometrical-optics approximation of emssion propagation in front of the region converts to the vacuum approximation behind it. The latter means that the linear-mode coupling in the Jovian inner magnetosphere is manifested as the effect of limiting polarization. Sources of decameter emission emitting at different frequencies f are located at heights corresponding to gyrofrequency levels f _Be ≅f and at magnetic-force lines that belong to L-shells passing through the satellite Io. The location of the transitional region in the Jovian magnetosphere varies depending on the emission frequency and the time. For each given decameter radio emission storm occupying some region in frequencytime space, we have a number of transitional regions located in a certain region of the Jovian magnetosphere—the interaction region of the magnetosphere (IRM) for the given emission storm. The distribution of magnetospheric plasma in an IRM is found from data of observations of the polarization ellipiicity of the given decameter radio emission storm. By matching the calculated ellipticity of emission with the observed ellipticity at every point of frequency-time space of the emission dynamic spectrum one finds a recurrent relation between the local values of the magnetospheric plasma density N_c and the planetary magnetic field B in the IRM, which allows evaluation of the distribution of plasma density if a definite model of the Jovian magnetic field has been adopted. Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia; Space Research Institute, Austrian Academy of Sciences, Austria. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 41, No. 2, pp. 177–193, February, 1998.     

Instabilities and turbulence in a high pressure plasma carrying transversal current

The excitations of electromagnetic waves in a high pressure plasma, carrying current perpendicular to the applied magnetic field is investigated. We assume that the relative velocity of ions and electrons exceeds the thermal velocity of ions. We have pointed out, that the excitation of kinetic branches of oscillations whith high growth rates referred to the lower hybrid frequency is possible. The paper contains some estimations of the fluctuations level when the saturation occurs and of the limiting values of heated ion temperature.     

A Mechanism for Generation of the Solar Magnetic Field

We apply the mathematical technique of quantum mechanics for studying the process of solar magnetic field generation under conditions where the viscosity is negligible and the rotation velocity of the medium is independent of time. It is assumed that the magnetic field is almost toroidal, axially nonsymmetric, and antisymmetric with respect to the equatorial plane.We show that in the presence of an axisymmetric poloidal component of the hydrodynamic velocity and a radial gradient of the angular velocity of the medium, an oscillating solution growing in time exists for the field. The characteristic frequency of oscillations can exceed the rotation frequency if the rotation of the medium is nonuniform. In the case where the characteristic time of field growth amounts to 10 years, the radial velocity of the medium in the field-generation zone is approximately equal to 10 cm/sec. We also discuss briefly the problem of the existence of two field-generation zones.     

On the Gradient-Current Mechanism of Formation of the Irregular Structure of the High-Latitude Upper Ionosphere

We consider the gradient-current instability of an inhomogeneous magnetoactive plasma in the approximation of double-fluid magnetohydrodynamics. Unlike the known gradient-drift and current-convective instabilities, the gradient-current instability is related to generation of nonpotential quasistatic electric fields polarized orthogonal to the external magnetic field B ₀ and excited by eddy currents whose density vector lies in the plane passing through the vectors of the magnetic field B ₀ and large-scale electron-density gradient. It is shown that in the high-latitude upper ionosphere, in the regions containing large-scale currents flowing in and out of the ionosphere along the magnetic field, the gradient-current instability can lead to the appearance of sheet-like irregularities extended predominantly in the plane passing through the geomagnetic-field and regular plasma-drift velocity vectors. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 48, No. 7, pp. 574–587, August 2005.     

A steadily rotating plasma disk

A homogeneously rotating plasma disk can be formed in a radially directed Ar-arc discharge at reduced pressure with an externally applied axial magnetic field. The radial pressure distribution is measured, as well as the emitted continuum radiation and the arc voltage. With these experimental values profiles of temperature, radial and azimuthal current density, and flow velocity in the disk are evaluated. Viscosity determines the flow pattern essentially. The effects of magnetic field and rotational motion on the discharge are investigated. The disk exhibits at nonrigid rotation a strong centrifugal force and a minor Coriolis force. A weak double vortex is found to develop in the meridional plane. The electric field in the discharge is altered by the azimuthal plasma flow.     

感应式脉冲推力器中等离子体加速数值研究

为了分析感应式脉冲放电等离子体推力器中时变电磁场作用下等离子体的放电参数分布及其随着磁场强度变化的影响,引入了利用双曲型散度清除方法的二维轴对称瞬态等离子体流动的磁流体力学数值模型.计算结果表明,随着输入能量的增加,等离子体团出现速度峰值的时刻提前,等离子体中同时存在的异号电流环对其加速具有阻滞作用.等离子体的加速效率随着磁场强度非线性增大,磁场大于某一临界值时(几何构型下峰值磁场强度大于0.45 T),有限空间情况下等离子体的加速效率获得显著提高.     

Emission Intensity Enhancement of DC Arc Plasma Induced by External Oscillating Magnetic Field

Direct current (dc) arc plasma with continuous aerosol supply was coupled with an external oscillatingmagnetic field of a few tens of mT and a frequency of up to 1 kHz. Such configuration was used to alter the plasma‐related radiative properties. The magnetic field was oriented perpendicularly to the electric field in the plasma and forced the arc column to oscillate as a whole with respect to the surrounding atmosphere. The magnitude of the appliedmagnetic.eld controls the amplitude of the oscillatory motion. Several parameters that can contribute to the radiative properties of the plasma were investigated (arc current, composition of aerosol introduced into the plasma, amplitude and frequency of the magnetic field applied). Spectral emission from different zones of the plasma column was measured by optical emission spectroscopy (OES). In comparison to steady‐state plasma, the applied magnetic field induces an intensity enhancement of emission of the most analytes considered. The intensity enhancement is strongly affected by the amplitude and frequency of plasma column oscillations, i.e. by plasma column velocity. Also, intensity enhancement depends on the plasma zone observed. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

外加磁场微波等离子推力器内流场数值模拟

为了提高微波等离子推力器性能，改善等离子体对电磁波能量的吸收状况，提高核心区温度，提出外加磁场的方案，并对热等离子体进行了数值模拟.假设局域热平衡条件，采用Navier-Stokes，Maxwell和Saha方程，利用压力修正的半隐格式和时域有限差分求解方法，建立了径向磁镜场下推力器内等离子体流场的数值计算模型.数值模拟结果表明：外加磁场后的磁感应强度小于0.5 T时，推力器内热等离子体核心区最高温度随磁感应强度的增加而迅速提高.外加磁场后的磁感应强度大于0.5 T时，核心区最高温度随磁感应强度的增加而缓慢提高.磁感应强度为0.5 T时，热等离子体核心区最高温度与不加磁场相比提高了24%.外加磁场对等离子体流场速度分布影响不大. 关键词： 等离子体模拟 等离子体相互作用 等离子体流动     

Formation and transportation of low-energy high-current electron beams in the plasma-filled diode under the effect of the external magnetic field

The mechanisms behind limitation of current of nonrelativistic high-current electron beams in the plasma-filled diode immersed in the external guiding magnetic field whose intensity is comparable with that of the beam self magnetic field are studied. It is shown that the beam current is limited by transmission capacity of the double layer between the cathode and anode plasma on the one hand and, on the other hand, by charge neutralization of the beam and by the decrease of the longitudinal velocity of the beam electrons under the action of the induced electric field and of the beam self magnetic field. The effect of the beam self fields on its cross-sectional current density and energy distributions is studied. Results of the numerical simulations are in good agreement with the experimental data.