Journal articles: 'Alfven waves-Magnetized plasmas'

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Sallago, P. A. "STABILITY OF ALFVEN WINGS IN HMHD." Anales AFA 32, no. 1 (April 15, 2021): 1–6. http://dx.doi.org/10.31527/analesafa.2021.32.1.1.

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A conducting source moving uniformly through a magnetized plasma generates, among a variety of perturbations,Alfvén waves. Alfvén waves can build up structures in the plasma called Alfvén wings. The wings have been detec-ted and measured in many solar system bodies, and their existence have been theoretically proved also. Under certainconditions, Hall and electronic pressure must be taken into account in the Ohm’s law and so one gets Hall Magne-tohydrodynamics (HMHD). In spite of Sallago and Platzeck have shown the existence of Alfvén wings in HMHD, theirstability under such conditions remains to be studied. The aim of this paper is to analyze the stability of an Alfvén wing,in the presence of an incompressible perturbation that has the same symmetry than the structure and polarization, inHMHD. Palumbo has developed an analytical method for the study of the stability of static structures with a symmetryin magnetized plasmas, in the presence of incompressible perturbations with the same symmetry than the structure.Since Alfvén wings are stationary structures, Sallago and Platzeck have shown the stability of such Alfvén wings in MHD conditions by extending Palumbo’s method. In the present paper this method is extended for Alfvén wings in HMHD conditions, and one concludes that in the presence of this kind of perturbations they are stable.

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Tishchenko, Vladimir, Artem Berezutsky, Leila Dmitrieva, Ilya Miroshnichenko, and Ildar Shaikhislamov. "Generation of Alfvén waves in magnetized plasma by laser plasma bunches at Mach numbers much less than unity." Solar-Terrestrial Physics 8, no. 2 (June 30, 2022): 91–97. http://dx.doi.org/10.12737/stp-82202214.

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In this paper, we examine a torsional Alfvén wave produced by periodic plasma bunches in a magnetized plasma flux tube. A new effect has been revealed: the wave is generated not only during the action of bunches, but also for a long time after the termination, which makes it possible to increase the wavelength by several times. We have determined the conditions under which the wave contains η~40 % of the total bunch energy. The wave radius depends on the energy of one bunch; and the length, on their number. The optimum number of bunches is 15. Simultaneously with the Alfvén wave, a bunch plasma jet (η~35 %) and a slow magnetosonic wave (η~10 %) propagate in the force tube. Similarity parameters scale the results to laboratory and near-Earth magnetized plasma.

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Cramer, N. F. "Alfvén resonance absorption in electron-positron plasmas." Proceedings of the International Astronomical Union 6, S274 (September 2010): 224–27. http://dx.doi.org/10.1017/s1743921311006983.

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AbstractWaves propagating obliquely in a magnetized cold pair plasma experience an approximate resonance in the wavevector component perpendicular to the magnetic field, which is the analogue of the Alfvén resonance in normal electron-ion plasmas. Wave absorption at the resonance can take place via mode conversion to the analogue of the short wavelength inertial Alfvén wave. The Alfvén resonance could play a role in wave propagation in the pulsar magnetosphere leading to pulsar radio emission. Ducting of waves in strong plasma gradients may occur in the pulsar magnetosphere, which leads to the consideration of Alfvén surface waves, whose energy is concentrated in the region of strong gradients.

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Wang, L. P., Z. B. Guo, Z. J. Mao, and Y. Zhang. "Phase finite time singularity: On the dissolution of a surface MHD eigenmode to the Alfvén continuum." Physics of Plasmas 30, no. 3 (March 2023): 032105. http://dx.doi.org/10.1063/5.0132609.

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Phase mixing is a general mechanism of collisionless damping in magnetized plasmas. In a MHD model, the carrier of phase mixing is the Alfvén wave continuum, which is driven by the plasma inhomogeneity. In this work, we study the non-resonant conversion of a surface MHD eigenmode to the Alfvén continuum. It is shown that the finite-time-singularity of the phase of the surface mode can smear its periodic oscillation and induces the excitation of the local Alfvén waves. This type of mode conversion would enhance the collisionless dissipation of the surface eigenmode, i.e., accelerating its dissolution to the Alfvén continuum. The non-resonant mode conversion and damping mechanism explored here have potential applications to understand the physics of collisionless dissipation of various eigenmodes in magnetized plasmas.

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SALLAGO, P. A., and A. M. PLATZECK. "Stability of Alfvén wings in uniform plasmas." Journal of Plasma Physics 73, no. 6 (December 2007): 957–66. http://dx.doi.org/10.1017/s0022377807006460.

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AbstractA conducting source moving uniformly through a magnetized plasma generates, among a variety of perturbations, Alfvén waves. An interesting characteristic of Alfvén waves is that they can build up structures in the plasma called Alfvén wings. These wings have been detected and measured in many solar system bodies, and their existence has also been theoretically proven. However, their stability remains to be studied. The aim of this paper is to analyze the stability of an Alfvén wing developed in a uniform background field, in the presence of an incompressible perturbation that has the same symmetry as the Alfvén wing, in the magnetohydrodynamic approximation. The study of the stability of a magnetohydrodynamic system is often performed by linearizing the equations and using either the normal modes method or the energy method. In spite of being applicable for many problems, both methods become algebraically complicated if the structure under analysis is a highly non-uniform one. Palumbo has developed an analytical method for the study of the stability of static structures with a symmetry in magnetized plasmas, in the presence of incompressible perturbations with the same symmetry as the structure (Palumbo 1998 Thesis, Universidad de Firenze, Italia). In the present paper we extend this method for Alfvén wings that are stationary structures, and conclude that in the presence of this kind of perturbation they are stable.

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Muñoz, V., F. A. Asenjo, M. Domínguez, R. A. López, J. A. Valdivia, A. Viñas, and T. Hada. "Large-amplitude electromagnetic waves in magnetized relativistic plasmas with temperature." Nonlinear Processes in Geophysics 21, no. 1 (February 14, 2014): 217–36. http://dx.doi.org/10.5194/npg-21-217-2014.

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Abstract. Propagation of large-amplitude waves in plasmas is subject to several sources of nonlinearity due to relativistic effects, either when particle quiver velocities in the wave field are large, or when thermal velocities are large due to relativistic temperatures. Wave propagation in these conditions has been studied for decades, due to its interest in several contexts such as pulsar emission models, laser-plasma interaction, and extragalactic jets. For large-amplitude circularly polarized waves propagating along a constant magnetic field, an exact solution of the fluid equations can be found for relativistic temperatures. Relativistic thermal effects produce: (a) a decrease in the effective plasma frequency (thus, waves in the electromagnetic branch can propagate for lower frequencies than in the cold case); and (b) a decrease in the upper frequency cutoff for the Alfvén branch (thus, Alfvén waves are confined to a frequency range that is narrower than in the cold case). It is also found that the Alfvén speed decreases with temperature, being zero for infinite temperature. We have also studied the same system, but based on the relativistic Vlasov equation, to include thermal effects along the direction of propagation. It turns out that kinetic and fluid results are qualitatively consistent, with several quantitative differences. Regarding the electromagnetic branch, the effective plasma frequency is always larger in the kinetic model. Thus, kinetic effects reduce the transparency of the plasma. As to the Alfvén branch, there is a critical, nonzero value of the temperature at which the Alfvén speed is zero. For temperatures above this critical value, the Alfvén branch is suppressed; however, if the background magnetic field increases, then Alfvén waves can propagate for larger temperatures. There are at least two ways in which the above results can be improved. First, nonlinear decays of the electromagnetic wave have been neglected; second, the kinetic treatment considers thermal effects only along the direction of propagation. We have approached the first subject by studying the parametric decays of the exact wave solution found in the context of fluid theory. The dispersion relation of the decays has been solved, showing several resonant and nonresonant instabilities whose dependence on the wave amplitude and plasma temperature has been studied systematically. Regarding the second subject, we are currently performing numerical 1-D particle in cell simulations, a work that is still in progress, although preliminary results are consistent with the analytical ones.

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Brodin, G., and L. Stenflo. "Three-wave coupling coefficients for magnetized plasmas with pressure anisotropy." Journal of Plasma Physics 41, no. 1 (February 1989): 199–208. http://dx.doi.org/10.1017/s0022377800013763.

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In order to find the equations for the nonlinear energy exchange between low-frequency waves in magnetized plasmas in the presence of pressure anisotropy, we start from the Chew–Goldberger–Low equations, the isothermal MHD equations, as well as a new hybrid system of equations. The coupling coefficients describing the interaction between two Alfvén waves and one magnetosonic wave as well as the interaction between two magnetosonic waves and one Alfvén wave are deduced.

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MELROSE, D. B., M. E. GEDALIN, M. P. KENNETT, and C. S. FLETCHER. "Dispersion in an intrinsically relativistic, one-dimensional, strongly magnetized pair plasma." Journal of Plasma Physics 62, no. 2 (August 1999): 233–48. http://dx.doi.org/10.1017/s0022377899007795.

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The properties of a relativistic plasma dispersion function (RPDF) for an intrinsically extremely relativist, strongly magnetized, one-dimensional, electron–positron plasma are discussed in detail. For a plasma with a mean Lorentz factor 〈γ〉 [Gt ] 1 in its rest frame, the RPDF has a large peak >〈γ〉 at a phase speed a fraction of order 1/〈γ〉 below the speed of light, and the asymptotic value (infinite phase speed) is 〈γ−3〉 ∼ 1/〈γ〉. These features are not particularly sensitive to the choice of distribution function. The RPDF is used to discuss the properties of waves in such plasmas. Particular points discussed are the implications of the RPDF for the maximum frequency for parallel Langmuir waves, and for the reconnection between the Langmuir mode and the Alfvén mode.

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Berezutsky, A. G., V. N. Tishchenko, A. A. Chibranov, I. B. Miroshnichenko, Yu P. Zakharov, and I. F. Shaikhislamov. "Controlling the type and intensity of low-frequency waves generated by laser plasma clots in a force tube of magnetized plasma." Journal of Physics: Conference Series 2067, no. 1 (November 1, 2021): 012019. http://dx.doi.org/10.1088/1742-6596/2067/1/012019.

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Abstract In this work, we study the influence of the parameters of a magnetized background plasma on the intensity of whistler waves generated by periodic laser plasma bunches in a magnetic field tube. It is shown that at 0.3 < Lpi > 0.4 Alfvén waves and whistlers are generated. In the region Lpi> 0.5, intense whistlers with an amplitude of δBmax / B0 ∼ 0.24 are generated.

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Cramer, N. F., and S. V. Vladimirov. "Alfvén surface waves in a magnetized dusty plasma." Physics of Plasmas 3, no. 12 (December 1996): 4740–47. http://dx.doi.org/10.1063/1.872041.

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Ishaq, Muhammad, and Hang Xu. "Nonlinear dispersive Alfvén waves interaction in magnetized plasma." Physics of Fluids 31, no. 8 (August 2019): 082105. http://dx.doi.org/10.1063/1.5106395.

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HUANG, GUANG-LI, and REN-YING WANG. "The growth of Alfvén waves in the resistive current-driven instability." Journal of Plasma Physics 58, no. 3 (October 1997): 433–40. http://dx.doi.org/10.1017/s0022377897006089.

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On the basis of a two-fluid, cold-plasma, linear stability calculation with linear friction between electrons and ions, the growth rate of Alfvén waves is derived from the dispersion relation for a uniformly magnetized plasma, in which the plasma resistivity and a uniform electric current carried by an electron beam are both considered. The growth rate is directly proportional to the plasma resistivity, the electric current density and the value of the parameter ωxpe/Ωe (where ωxpe and Ωe are the electron plasma and cyclotron frequency respectively). Moreover, the growth of Alfvén waves is mainly excited in a direction nearly parallel to the ambient magnetic field. The critical value of the velocity of the electron fluid is just equal to the Alfvén velocity. The results of this paper are compared with those for the linear tearing mode.

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Shukla, P. K., and R. Bharuthram. "Convective cell and Alfvén vortices in an inhomogeneous rotating cold magnetoplasma." Journal of Plasma Physics 37, no. 2 (April 1987): 199–208. http://dx.doi.org/10.1017/s0022377800012113.

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It is shown that double vortices are a special class of stationary solutions of the set of nonlinear equations that governs the dynamics of modified convective cells and shear Alfvén waves in a cold rotating magnetized plasma. Criteria for the existence of dipole vortices as well as several analytical expressions for the vortex profiles are presented. It is suggested that modified convective cell and Alfvén dipole vortices may cause anomalous cross-field particle transport in a low-β plasma, such as the ionosphere.

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Rajib, T. I., S. Sultana, and A. A. Mamun. "Shear Alfvén Waves in a Magnetized Electron–Positron Plasma." IEEE Transactions on Plasma Science 46, no. 7 (July 2018): 2612–18. http://dx.doi.org/10.1109/tps.2017.2772024.

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Yukhimuk, A. K., O. G. Fal'ko, V. A. Yukhimuk, V. P. Kucherenko, and V. N. Fedun. "Nonlinear interection of alfven waves and ionic acoustic waves in a magnetized plasma." Kosmìčna nauka ì tehnologìâ 2, no. 3-4 (May 30, 1996): 44–48. http://dx.doi.org/10.15407/knit1996.03.044.

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Rubab, N., and G. Jaffer. "Quantum Treatment of Kinetic Alfvén Waves Instability in a Dusty Plasma: Magnetized Ions." Advances in High Energy Physics 2016 (2016): 1–6. http://dx.doi.org/10.1155/2016/6793572.

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Kinetic Alfvén wave instability is examined rigorously in a uniform nondegenerate quantum dusty plasma. A linear dispersion relation of kinetic Alfvén wave in inertial regime is derived by incorporating Bohm potential in the linearized Vlasov model. It is found that the quantum correctionCQappears due to the insertion of Bohm potential in Vlasov model and causes the suppression in the Alfvén wave frequency and the growth rates of instability. A number of analytical expressions for various modes of propagation are derived. It is also found that the system parameters, that is, streaming velocity, dust charge, number density, and quantum correction, significantly influence the dispersion relation and the growth rate of instability.

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De Toni, L. B., R. Gaelzer, and L. F. Ziebell. "Oblique Alfvén waves in a stellar wind environment with dust particles charged by inelastic collisions and by photoionization." Monthly Notices of the Royal Astronomical Society 512, no. 2 (February 28, 2022): 1795–804. http://dx.doi.org/10.1093/mnras/stac547.

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ABSTRACT The characteristics of Alfvén waves propagating in a direction oblique to the ambient magnetic field in a stellar wind environment are discussed. A kinetic formulation for a magnetized dusty plasma is adopted considering Maxwellian distributions of electrons and ions, and immobile dust particles electrically charged by absorption of plasma particles and by photoionization. The dispersion relation is numerically solved and the results are compared with situations previously studied where dust particles were not charged by photoionization, which is an important process in a stellar wind of a relatively hot star. We show that the presence of dust causes the shear Alfvén waves to present a region of wavenumber values with zero frequency and that the minimum wavelength for which the mode becomes dispersive again is roughly proportional to the radiation intensity to which the dust grains are exposed. The damping rates of both shear and compressional Alfvén waves are observed to decrease with increasing radiation flux, for the parameters considered. For the particular case where both modes present a region with null real frequency when the radiation flux is absent or weak, it is shown that when the radiation flux is sufficiently strong, the photoionization mechanism may cause this region to get smaller or even to vanish, for compressional Alfvén waves. In that case, the compressional Alfvén waves present non-zero frequency for all wavenumber values, while the shear Alfvén waves still present null frequency in a certain interval of wavenumber values, which gets smaller with the presence of radiation.

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Panwar, A., C. M. Ryu, and A. S. Bains. "Kinetic Alfven solitary waves in a magnetized plasma with superthermal electrons." Physics of Plasmas 22, no. 9 (September 2015): 092130. http://dx.doi.org/10.1063/1.4931993.

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BANDYOPADHYAY, ANUP, and K. P. DAS. "Higher-order growth rate of instability of obliquely propagating kinetic Alfvén and ion-acoustic solitons in a magnetized non-thermal plasma." Journal of Plasma Physics 68, no. 4 (May 2002): 285–303. http://dx.doi.org/10.1017/s002237780200199x.

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The higher-order growth rate of instability for obliquely propagating kinetic Alfvén and ion-acoustic solitons in a magnetized non-thermal plasma have been obtained by the multiple-scale perturbation expansion method developed by Allen and Rowlands (1993). The growth rate of instability is obtained correct to order k2, where k is the wave number of a long-wavelength plane-wave perturbation. The corresponding lowest-order stability analysis has been considered recently by Bandyopadhyay and Das (2000b). It has been found that the kinetic Alfvén solitary waves are stable at the order of k but are unstable at the order of k2. It has also been found that the growth rate of instability at the order of k for ion-acoustic solitary waves is free from the parameters of the non-thermal plasma but at the order of k2 depends on the parameters of the non-thermal plasma.

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Gorbachev, L. P. "Magnetoacoustic and Alfven waves excited by plasma cloud expansion in cold magnetized plasma." Radiophysics and Quantum Electronics 36, no. 9 (September 1993): 606–12. http://dx.doi.org/10.1007/bf01038204.

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SHUKLA, P. K., and L. STENFLO. "Nonlinear interactions between upper-hybrid and Alfvén modes in a magnetized plasma containing charged dust impurities." Journal of Plasma Physics 73, no. 1 (February 2007): 3–8. http://dx.doi.org/10.1017/s0022377806004740.

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Abstract.We consider the nonlinear interactions between upper-hybrid (UH) and Alfvén modes in a magnetized electron–ion plasma containing a fraction of stationary charged dust grains. The interaction is governed by a pair of equations for the UH wave envelope including the relativistic electron mass increase and the density and compressional magnetic field fluctuations associated with the Alfvén modes that are, in turn, driven by the ponderomotive force of the UH waves. The coupled mode equations are then Fourier analyzed to obtain a new dispersion relation, which admits new classes of modulational instabilities. The existence of a cusp-shaped UH envelope soliton is also predicted. The result can have relevance to the electron acceleration by sharply localized UH waves in the dusty magnetosphere of Saturn.

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YUKHIMUK, A. K., V. A. YUKHIMUK, O. K. SIRENKO, and Yu M. VOITENKO. "Parametric excitation of electromagnetic waves in a magnetized plasma." Journal of Plasma Physics 62, no. 1 (July 1999): 53–64. http://dx.doi.org/10.1017/s0022377899007709.

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The parametric interaction of an upper-hybrid pump wave with kinetic Alfvén and electromagnetic waves that propagate in parallel and perpendicular directions to the ambient magnetic field is investigated on the basis of two-fluid magnetohydrodynamics. A nonlinear dispersion relation describing three-wave interaction and instability growth rates are found. The theoretical results are used for the interpretation of satellite observations in the magnetospheric plasma. It is shown that as a result of the decay of an upper-hybrid wave, electromagnetic waves propagating in both parallel and perpendicular directions to the ambient magnetic field are generated. The instability growth rate is much higher in the case of left-polarized electromagnetic wave generation than in the case of ordinary electromagnetic wave generation. The nonlinear parametric processes studied here could also take place during powerful bursts on the Sun, and in the magnetosphere of Jupiter.

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ZHANG, T. X. "Anisotropic model for resonant heating of ions by Alfvén waves." Journal of Plasma Physics 79, no. 5 (August 9, 2013): 963–71. http://dx.doi.org/10.1017/s0022377813000871.

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AbstractAnisotropic heating of ions by Alfvén waves with frequency in the ion–cyclotron frequency range and propagation parallel to the magnetic field lines is investigated. First, particle–Alfvén wave interactions are quasilinearly examined from the kinetic theory in a hot multi-ion-magnetized plasma. As a result, the parallel and perpendicular heating rates of ions are derived analytically. Then, in terms of this anisotropic heating model and the dispersion relation of magnetic field-aligned left-hand polarized electromagnetic ion–cyclotron–Alfvén (EMICA) waves, the resonant heating of H, 2H, 3H, 3He, and 4He ions in a typical preheated laboratory plasma is numerically studied. It is shown that the EMICA waves can efficiently heat ions through cyclotron resonances primarily in the perpendicular direction. The perpendicular temperatures of H, 2H, 3H, 3He, and 4He increase much faster than the parallel ones. In comparison with the result from the previously developed isotropic heating model, the parallel heating by the EMICA waves is about much weaker, while the perpendicular heating is more efficient. Parameters such as density, temperature, magnetic field, wave-energy density, and ion species can affect the efficiency of the Alfvén wave heating in a similar way as shown in the isotropic heating model. The anisotropic model can be applied to explain the measurements of why O+5 and Mg+9 are heated extreme perpendicularly in solar coronal holes.

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Vladimirov, S. V., and N. F. Cramer. "Nonlinear Alfvén waves in magnetized plasmas with heavy impurities or dust." Physical Review E 54, no. 6 (December 1, 1996): 6762–68. http://dx.doi.org/10.1103/physreve.54.6762.

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Wessen, K. P., and N. F. Cramer. "Finite-frequency surface waves on current sheets." Journal of Plasma Physics 45, no. 3 (June 1991): 389–406. http://dx.doi.org/10.1017/s0022377800015798.

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The dispersion relation for low-frequency surface waves at a current sheet between two magnetized plasmas is derived using the cold-plasma dielectric tensor with finite ion-cyclotron frequency. The magnetic field direction is allowed to change discontinuously across the sheet, but the plasma density remains constant. The cyclotron frequency causes a splitting of the dispersion relation into a number of mode branches with frequencies both less than and greater than the ion-cyclotron frequency. The existence of these modes depends in particular upon the degree of magnetic field discontinuity and the direction of wave propagation in the sheet relative to the magnetic field directions. Sometimes two modes can exist for the same direction of propagation. The existence of modes undamped by Alfvén resonance absorption is predicted. Analytical solutions are obtained in the low-frequency and magnetic-field-reversal limits. The solutions are obtained numerically in the general case.

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Прокопов, Павел, Pavel Prokopov, Юрий Захаров, Yuriy Zakharov, Владимир Тищенко, Vladimir Tishchenko, Эдуард Бояринцев, et al. "On the possibility for laboratory simulation of generation of Alfven disturbances in magnetic tubes in the solar atmosphere." Solnechno-Zemnaya Fizika 2, no. 1 (March 17, 2016): 14–23. http://dx.doi.org/10.12737/13481.

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The paper deals with generation of Alfven plasma disturbances in magnetic flux tubes through exploding laser plasma in magnetized background plasma. Processes with similar effect of excitation of torsion-type waves seem to provide energy transfer from the solar photosphere to corona. The studies were carried out at experimental stand KI-1 represented a high-vacuum chamber of 1.2 m diameter, 5 m long, external magnetic field up to 500 Gs along the chamber axis, and up to 2·10–6 Torr pressure in operating mode. Laser plasma was produced when focusing the CO2 laser pulse on a flat polyethylene target, and then the laser plasma propagated in θ-pinch background hydrogen (or helium) plasma. As a result, the magnetic flux tube of 15–20 cm radius was experimentally simulated along the chamber axis and the external magnetic field direction. Also, the plasma density distribution in the tube was measured. Alfven wave propagation along the magnetic field was registered from disturbance of the magnetic field transverse component Bφ and field-aligned current Jz. The disturbances propagate at near-Alfven velocity of 70–90 km/s and they are of left-hand circular polarization of the transverse component of magnetic field. Presumably, Alfven wave is generated by the magnetic laminar mechanism of collisionless interaction between laser plasma cloud and background. The right-hand polarized high-frequency whistler predictor was registered which have been propagating before Alfven wave at 300 km/s velocity. The polarization direction changed with Alfven wave coming. Features of a slow magnetosonic wave as a sudden change in background plasma concentration along with simultaneous displacement of the external magnetic field were found. The disturbance propagates at ~20–30 km/s velocity, which is close to that of ion sound at low plasma beta value. From preliminary estimates, the disturbance transfers about 10 % of the original energy of laser plasma.

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Rajib, T. I., and S. Sultana. "Propagation of Compressional Alfvén Waves in a Magnetized Pair Plasma Medium." AIP Advances 12, no. 6 (June 1, 2022): 065318. http://dx.doi.org/10.1063/5.0089738.

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The reductive perturbation approach was used to explore the nonlinear propagation of fast (compressive) and slow (rarefactive) electron–positron (EP) magnetoacoustic (EPMA) modes in an EP plasma medium. The solitary wave solution of the Korteweg-de Vries (K-dV) equation is used to identify the basic properties of EP compressional Alfvén waves. It is shown that the fast (slow) EPMA mode is predicted to propagate as compressive (rarefactive) solitary waves. The basic features (i.e., speed, amplitude, and width) of the compressive (i.e., fast) EPMA waves are found to be completely different from those of rarefactive (i.e., slow) EPMA ones. It is also examined that hump (dip) shape solitary waves are found for the fast (slow) mode. The significance of our findings is in understanding the nonlinear electromagnetic wave phenomena in laboratory plasma and space environments where EP plasma may exist.

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Ruan, Shi-Sen, and Zhong-Ming Li. "Head-on collision of dust magnetoacoustic solitary waves in magnetized plasmas." Journal of Plasma Physics 80, no. 2 (December 13, 2013): 235–45. http://dx.doi.org/10.1017/s0022377813001244.

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AbstractThe head-on collision of dust magnetoacoustic solitary waves (DMASWs) is studied in magnetized electron–ion–dust plasma. The extended Poincaré–Lighthill–Kuo perturbation method is used to derive the Korteweg de Vries equations for DMASWs in this three-component plasma. The effects of the magnetic field intensity B0, the number of electrons residing on dust surface Zd, the ratio of electron to dust number density δ, the ratio of electron to ion temperature σ, and the ratio of dust acoustic velocity to dust Alfvén velocity β on the phase shift are investigated. It is found that these parameters can significantly influence the phase shifts of colliding DMASWs. The present investigation may be beneficial to understand the interaction between two DMASWs that may occur in plasma with dust impurities situations.

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Кичигин, Геннадий, and Gennadiy Kichigin. "Structure of nonlinear whistlers moving through plasma at an angle to the magnetic field." Solar-Terrestrial Physics 4, no. 1 (March 31, 2018): 25–28. http://dx.doi.org/10.12737/stp-41201803.

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The paper presents solutions of two-fluid magnetic hydrodynamics equations describing small-scale fast magnetosonic stable waves — nonlinear whist-lers moving in a cold magnetized plasma at an angle α to the external magnetic field. At the fixed angle α, the Alfvén Mach number of the whistlers has a narrow range of allowed values. It has been found that when passing from extremely small Mach numbers to ex-tremely large ones, amplitudes and spatial structure of wave velocity components and whistler magnetic field change significantly. The range of angles of the motion direction of whistlers with respect to direction of the the external magnetic field vector is determined. Within this range, the obtained approximate analytical and numerical solutions are in satisfactory agreement.

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Kempski, Philipp, Eliot Quataert, and Jonathan Squire. "Sound-wave instabilities in dilute plasmas with cosmic rays: implications for cosmic ray confinement and the Perseus X-ray ripples." Monthly Notices of the Royal Astronomical Society 493, no. 4 (February 24, 2020): 5323–35. http://dx.doi.org/10.1093/mnras/staa535.

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ABSTRACT Weakly collisional, magnetized plasmas characterized by anisotropic viscosity and conduction are ubiquitous in galaxies, haloes, and the intracluster medium (ICM). Cosmic rays (CRs) play an important role in these environments as well, by providing additional pressure and heating to the thermal plasma. We carry out a linear stability analysis of weakly collisional plasmas with CRs using Braginskii MHD for the thermal gas. We assume that the CRs stream at the Alfvén speed, which in a weakly collisional plasma depends on the pressure anisotropy (Δp) of the thermal plasma. We find that this Δp dependence introduces a phase shift between the CR-pressure and gas-density fluctuations. This drives a fast-growing acoustic instability: CRs offset the damping of acoustic waves by anisotropic viscosity and give rise to wave growth when the ratio of CR pressure to gas pressure is ≳αβ−1/2, where β is the ratio of thermal to magnetic pressure, and α, typically ≲1, depends on other dimensionless parameters. In high-β environments like the ICM, this condition is satisfied for small CR pressures. We speculate that the instability studied here may contribute to the scattering of high-energy CRs and to the excitation of sound waves in galaxy-halo, group and cluster plasmas, including the long-wavelength X-ray fluctuations in Chandra observations of the Perseus cluster. It may also be important in the vicinity of shocks in dilute plasmas (e.g. cluster virial shocks or galactic wind termination shocks), where the CR pressure is locally enhanced.

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31

Shaikh, D., and P. K. Shukla. "Spectral properties of electromagnetic turbulence in plasmas." Nonlinear Processes in Geophysics 16, no. 2 (March 12, 2009): 189–96. http://dx.doi.org/10.5194/npg-16-189-2009.

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Abstract. We report on the nonlinear turbulent processes associated with electromagnetic waves in plasmas. We focus on low-frequency (in comparison with the electron gyrofrequency) nonlinearly interacting electron whistlers and nonlinearly interacting Hall-magnetohydrodynamic (H-MHD) fluctuations in a magnetized plasma. Nonlinear whistler mode turbulence study in a magnetized plasma involves incompressible electrons and immobile ions. Two-dimensional turbulent interactions and subsequent energy cascades are critically influenced by the electron whisters that behave distinctly for scales smaller and larger than the electron skin depth. It is found that in whistler mode turbulence there results a dual cascade primarily due to the forward spectral migration of energy that coexists with a backward spectral transfer of mean squared magnetic potential. Finally, inclusion of the ion dynamics, resulting from a two fluid description of the H-MHD plasma, leads to several interesting results that are typically observed in the solar wind plasma. Particularly in the solar wind, the high-time-resolution databases identify a spectral break at the end of the MHD inertial range spectrum that corresponds to a high-frequency regime. In the latter, turbulent cascades cannot be explained by the usual MHD model and a finite frequency effect (in comparison with the ion gyrofrequency) arising from the ion inertia is essentially included to discern the dynamics of the smaller length scales (in comparison with the ion skin depth). This leads to a nonlinear H-MHD model, which is presented in this paper. With the help of our 3-D H-MHD code, we find that the characteristic turbulent interactions in the high-frequency regime evolve typically on kinetic-Alfvén time-scales. The turbulent fluctuation associated with kinetic-Alfvén interactions are compressive and anisotropic and possess equipartition of the kinetic and magnetic energies.

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LYUTIKOV, MAXIM. "Beam instabilities in a magnetized pair plasma." Journal of Plasma Physics 62, no. 1 (July 1999): 65–86. http://dx.doi.org/10.1017/s0022377899007837.

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Beam instabilities in the strongly magnetized electron–positron plasma of a pulsar magnetosphere are considered. We analyse the resonance conditions and estimate the growth rates of the Cherenkov and cyclotron instabilities of the ordinary (O), extraordinary (X) and Alfvén modes in two limiting regimes: kinetic and hydrodynamic. The importance of the different instabilities as a source of coherent pulsar radiation generation is then estimated, taking into account the angular dependence of the growth rates and the limitations on the length of the coherent wave–particle interaction imposed by the curvature of the magnetic field lines. We conclude that in the pulsar magnetosphere, Cherenkov-type instabilities occur in the hydrodynamic regime, while cyclotron-type instabilities occur in the kinetic regime. We argue that electromagnetic cyclotron-type instabilities on the X, O and probably Alfvén waves are more likely to develop in the pulsar magnetosphere.

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33

Laveder, D., T. Passot, and P. L. Sulem. "Fluid simulations of non-resonant anisotropic ion heating." Annales Geophysicae 31, no. 7 (July 9, 2013): 1195–204. http://dx.doi.org/10.5194/angeo-31-1195-2013.

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Abstract. The finite Larmor radius (FLR)-Landau fluid model, which extends the usual anisotropic magnetohydrodynamics to magnetized collisionless plasmas by retaining linear Landau damping and finite Larmor radius corrections down to the sub-ionic scales in the quasi-transverse directions, is used to study the non-resonant heating of the plasma by randomly driven Alfvén waves. One-dimensional numerical simulations, free from any artificial dissipation, are used to analyze the influence on the thermal dynamics, of the beta parameter and of the separation between the driving and the ion scales. While the gyrotropic heat fluxes play a dominant role when the plasma is driven at large scales, leading to a parallel heating of the ions by Landau damping, a different regime develops when the driving acts at scales comparable to the ion Larmor radius. Perpendicular heating and parallel cooling of the ions are then observed, an effect that is mostly due to the work of the non-gyrotropic pressure force and that can be viewed as the fluid signature of the so-called stochastic heating. A partial characterization of the plasma by global quantities (such as the magnetic compressibility and the density-magnetic field correlations that provide information on the dominant type of waves) is also presented. The enhancement of the parallel electron heating by a higher level of fast magnetosonic waves is in particular pointed out.

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34

Gary, S. Peter. "Low-frequency waves in a high-beta collisionless plasma: polarization, compressibility and helicity." Journal of Plasma Physics 35, no. 3 (June 1986): 431–47. http://dx.doi.org/10.1017/s0022377800011442.

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This paper considers the linear theory of waves near and below the ion cyclotron frequency in an isothermal electron-ion Vlasov plasma which is isotropic, homogeneous and magnetized. Numerical solutions of the full dispersion equation for the magnetosonic/whistler and Alfvén/ion cyclotron modes at βi = 1·0 are presented, and the polarizations, compressibilities, helicities, ion Alfvén ratios and ion cross-helicities are exhibited and compared. At sufficiently large βi and θ, the angle of propagation with respect to the magnetic field, the real part of the polarization of the Alfvén/ion cyclotron wave changes sign, so that, for such parameters, this mode is no longer left-hand polarized. The Alfvén/ion cyclotron mode becomes more compressive as the wavenumber ulereases, whereas the magnetosonic/whistler becomes more compressive with increasing θ, At oblique propagation, the helicity of both modes approaches zero in the long-wavelength limit; in contrast, the ion cross-helicity is of order unity for the Alfvén/ion cyclotron wave and decreases as θ increases for the magnetosonic/whistler mode.

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35

Salimullah, Mohammad, Brahmananda Dasgupta, and Kunihiko Watanabe. "Modification and Damping of Alfvén Waves in a Magnetized Dusty Plasma." Journal of the Physical Society of Japan 64, no. 10 (October 15, 1995): 3758–66. http://dx.doi.org/10.1143/jpsj.64.3758.

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Kourakis, I., and P. K. Shukla. "Linear and nonlinear properties of Rao-dust-Alfvén waves in magnetized plasmas." Physics of Plasmas 11, no. 3 (March 2004): 958–69. http://dx.doi.org/10.1063/1.1645793.

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Kavitha, L., C. Lavanya, V. Senthil Kumar, D. Gopi, and A. Pasqua. "Perturbed soliton excitations of Rao-dust Alfvén waves in magnetized dusty plasmas." Physics of Plasmas 23, no. 4 (April 2016): 043702. http://dx.doi.org/10.1063/1.4945609.

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38

Dewan, Himani, R. Uma, and R. P. Sharma. "Nonlinear evolution of Kinetic Alfvén Wave and the associated turbulence spectra in laser produced plasmas and laboratory simulation of astrophysical phenomena." Plasma Physics and Controlled Fusion 63, no. 12 (November 16, 2021): 125034. http://dx.doi.org/10.1088/1361-6587/ac35a4.

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Abstract This investigation presents the nonlinear interplay between pump wave (Kinetic Alfvén Wave (KAW)) and low-frequency ion acoustic wave (IAW) in the magnetized plasma. The model is developed by taking into account the ponderomotive nonlinearity associated due to the pump KAW. The coupled dimensionless equations (pump and IAW) are solved by adopting numerical simulation technique. The deduced results give the localization and filamentary structures of KAW, which eventually become chaotic with the evolution of time. The fundamental physics governing the dynamics of these two waves is influenced by the plasma beta ( β ) parameter; thereby affecting the nature of nonlinearity, dispersive properties and magnetic field amplification. The saturated spectra are analogous to that observed for many astrophysical scenarios for low (Chatterjee et al 2017 Nat. Commun. 8 15970) and high beta (White et al 2019 Nat. Commun. 10 1758; Tzeferacos et al 2017 Phys. Plasmas 24 041404) plasma. This theoretical model outlining the nonlinear interaction can be imperative in understanding the dynamics of magnetic field amplification in various astrophysical scenarios.

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Tishchenko, Vladimir, Artem Berezutsky, Leila Dmitrieva, Ilya Miroshnichenko, and Ildar Shaikhislamov. "Generation of Alfvén waves in magnetized plasma by laser plasma bunches at Mach numbers much less than unity." Solnechno-Zemnaya Fizika 8, no. 2 (June 30, 2022): 101–7. http://dx.doi.org/10.12737/szf-82202214.

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In this paper, we examine a torsional Alfvén wave produced by periodic plasma bunches in a magnetized plasma flux tube. A new effect has been revealed: the wave is generated not only during the action of bunches, but also for a long time after the termination, which makes it possible to increase the wavelength by several times. We have determined the conditions under which the wave contains η~40 % of the total bunch energy. The wave radius depends on the energy of one bunch; and the length, on their number. The optimum number of bunches is 15. Simultaneously with the Alfvén wave, a bunch plasma jet (η~35 %) and a slow magnetosonic wave (η~10 %) propagate in the force tube. Similarity parameters scale the results to laboratory and near-Earth magnetized plasma.

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Yukhimuk, A. K., V. N. Fedun, V. A. Yukhimuk, and V. N. Ivchenko. "Parametric excitation of upper hybrid and kinetic alfven waves in a magnetized plasma." Kosmìčna nauka ì tehnologìâ 4, no. 1 (January 30, 1998): 108–12. http://dx.doi.org/10.15407/knit1998.01.108.

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Das, K. P., L. P. J. Kamp, and F. W. Sluijter. "Three-dimensional stability of solitary shear kinetic Alfvén waves in a low-beta plasma." Journal of Plasma Physics 41, no. 1 (February 1989): 171–84. http://dx.doi.org/10.1017/s002237780001374x.

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The three-dimensional stability of solitary shear kinetic Alfvén waves in a low-β plasma is investigated by the method of Zakharov & Rubenchik (1974). It is found that there is no instability if the direction of perturbation falls within a certain region of space. The growth rate of the instability for the unstable region is determined. This growth rate is found to decrease with increasing angle between the direction of propagation of the solitary wave and the direction of the external uniform magnetic field. A particular case of the present analysis gives results on the stability of ion-acoustic solitons in a magnetized plasma.

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42

Kotsarenko, N. Ya, S. V. Koshevaya, and A. N. Kotsarenko. "Low frequency electromagnetic and kinetic Alfvén waves in a magnetized dusty plasma." Physica Scripta 56, no. 4 (October 1, 1997): 388–91. http://dx.doi.org/10.1088/0031-8949/56/4/009.

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Nakariakov, Valery M., and Dmitrii Y. Kolotkov. "Magnetohydrodynamic Waves in the Solar Corona." Annual Review of Astronomy and Astrophysics 58, no. 1 (August 18, 2020): 441–81. http://dx.doi.org/10.1146/annurev-astro-032320-042940.

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The corona of the Sun is a unique environment in which magnetohydrodynamic (MHD) waves, one of the fundamental processes of plasma astrophysics, are open to a direct study. There is striking progress in both observational and theoretical research of MHD wave processes in the corona, with the main recent achievements summarized as follows: ▪ Both periods and wavelengths of the principal MHD modes of coronal plasma structures, such as kink, slow and sausage modes, are confidently resolved. ▪ Scalings of various parameters of detected waves and waveguiding plasma structures allow for the validation of theoretical models. In particular, kink oscillation period scales linearly with the length of the oscillating coronal loop, clearly indicating that they are eigenmodes of the loop. Damping of decaying kink and standing slow oscillations depends on the oscillation amplitudes, demonstrating the importance of nonlinear damping. ▪ The dominant excitation mechanism for decaying kink oscillations is associated with magnetized plasma eruptions. Propagating slow waves are caused by the leakage of chromospheric oscillations. Fast wave trains could be formed by waveguide dispersion. ▪ The knowledge gained in the study of coronal MHD waves provides ground for seismological probing of coronal plasma parameters, such as the Alfvén speed, the magnetic field and its topology, stratification, temperature, fine structuring, polytropic index, and transport coefficients.

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Lakhin, V. P., S. V. Makurin, A. B. Mikhailovskii, and O. G. Onishchenko. "Dispersion ion-drift hydrodynamics." Journal of Plasma Physics 38, no. 3 (December 1987): 387–405. http://dx.doi.org/10.1017/s0022377800012678.

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The set of hydrodynamic equations for the ion component of a magnetized low-pressure plasma, including the nonlinear ion drift and waves related to it, taking into account dispersion effects of order k2⊥ρ2i (k⊥is the characteristic transverse wavenumber and ρi is the ion Larmor radius), is obtained. The reduction of these equations using the standard assumptions of vortex theory is given. The problem of the integrals of motion of the simplified equations is discussed. Account is taken of the gravitational force (which models curvature of the magnetic field lines), the three-dimensionality of the perturbations (drift-Alfvén effects) and plasma rotation. It is suggested that the ion-drift hydrodynamics discussed here should be the basis for the analysis of the ion drift and the vortices related to it, as well as for the theory of decay processes with participation of the ion-drift waves.

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45

Khattak, S. A., A. Mushtaq, and Qasim Jan. "Circularly polarized dust Alfvén solitary waves in magnetized gravitative-radiative quantum dusty plasma." Physics of Plasmas 26, no. 7 (July 2019): 072101. http://dx.doi.org/10.1063/1.5093312.

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Прокопов, Павел, Pavel Prokopov, Юрий Захаров, Yuriy Zakharov, Владимир Тищенко, Vladimir Tishchenko, Эдуард Бояринцев, et al. "On the possibility for laboratory simulation of generation of Alfvén disturbances in magnetic tubes in the solar atmosphere." Solar-Terrestrial Physics 2, no. 1 (June 1, 2016): 19–33. http://dx.doi.org/10.12737/19859.

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The paper deals with generation of Alfvén plasma disturbances in magnetic flux tubes through exploding laser plasma in magnetized background plasma. Processes with similar effect of excitation of torsion-type waves seem to provide energy transfer from the solar photosphere to the corona. The studies were carried out at experimental stand KI-1 representing a high-vacuum chamber 1.2 m in diameter, 5 m in length, external magnetic field up to 500 G along the chamber axis, and up to 2·10–6 Torr pressure in operating mode. Laser plasma was produced when focusing the CO2 laser pulse on a flat polyethylene target, and then the laser plasma propagated in θ-pinch background hydrogen (or helium) plasma. As a result, the magnetic flux tube 15–20 cm in radius was experimentally simulated along the chamber axis and the external magnetic field direction. Also, the plasma density distribution in the tube was measured. Alfvén wave propagation along the magnetic field was registered from disturbance of the magnetic field transverse component Bφ and field-aligned current Jz. The disturbances propagate at a near-Alfvén velocity 70–90 km/s and they are of left-hand circular polarization of the transverse component of magnetic field. Presumably, the Alfvén wave is generated by the magnetic laminar mechanism of collisionless interaction between laser plasma cloud and background. A right-hand polarized high-frequency whistler predictor was registered which propagated before the Alfvén wave at a velocity of 300 km/s. The polarization direction changed with the Alfvén wave coming. Features of a slow magnetosonic wave as a sudden change in background plasma concentration along with simultaneous displacement of the external magnetic field were found. The disturbance propagates at ~20–30 km/s velocity, which is close to that of ion sound at low plasma beta value. From preliminary estimates, the disturbance transfers about 10 % of the original energy of laser plasma.

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Кичигин, Геннадий, and Gennadiy Kichigin. "Structure of nonlinear whistlers moving through plasma at an angle to the magnetic field." Solnechno-Zemnaya Fizika 4, no. 1 (March 29, 2018): 28–32. http://dx.doi.org/10.12737/szf-41201803.

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The paper presents solutions of two-fluid magnetic hydrodynamics equations describing small-scale fast magnetosonic stable waves — nonlinear whist-lers moving in a cold magnetized plasma at an angle α to the external magnetic field. At the fixed angle α, the Alfvén Mach number of the whistlers has a narrow range of allowed values. It has been found that when passing from extremely small Mach numbers to ex-tremely large ones, amplitudes and spatial structure of wave velocity components and whistler magnetic field change significantly. The range of angles of the motion direction of whistlers with respect to direction of the the external magnetic field vector is determined. Within this range, the obtained approximate analytical and numerical solutions are in satisfactory agreement.

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Tanaka, Motohiko, Tetsuya Sato, and A. Hasegawa. "Excitation of kinetic Alfvén waves by resonant mode conversion and longitudinal heating of magnetized plasmas." Physics of Fluids B: Plasma Physics 1, no. 2 (February 1989): 325–32. http://dx.doi.org/10.1063/1.859145.

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49

Deconinck, Bernard, Peter Meuris, and Frank Verheest. "Oblique nonlinear Alfvén waves in strongly magnetized beam plasmas. Part 1. Nonlinear vector evolution equation." Journal of Plasma Physics 50, no. 3 (December 1993): 445–55. http://dx.doi.org/10.1017/s0022377800017268.

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Nonlinear MHD waves propagating obliquely to the external magnetic field in warm multi-species plasmas with anisotropic pressures and different equilibrium drifts are treated without imposing the customary quasi-neutrality between the different species or neglecting the displacement current in Ampère's law. The wave magnetic field obeys a vector nonlinear evolution equation, which in the limits of parallel propagation or of both the neglect of the displacement current and the imposition of quasi-neutrality reduces to the vector formulation of the well-known derivative nonlinear Schrödinger equation.

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Deconinck, Bernard, Peter Meuris, and Frank Verheest. "Oblique nonlinear Alfvén waves in strongly magnetized beam plasmas. Part 2. Soliton solutions and integrability." Journal of Plasma Physics 50, no. 3 (December 1993): 457–76. http://dx.doi.org/10.1017/s002237780001727x.

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Oblique propagation of MHD waves in warm multi-species plasmas with anisotropic pressures and different equilibrium drifts is described by a modified vector derivative nonlinear Schrödinger equation, if charge separation in Poisson's equation and the displacement current in Ampère's law are properly taken into account. This modified equation cannot be reduced to the standard derivative nonlinear Schrödinger equation, and hence requires a new approach to solitary-wave solutions, integrability and related problems. The new equation is shown to be integrable by the use of the prolongation method, and by finding a sufficient number of conservation laws, and possesses bright and dark soliton solutions, besides possible periodic solutions.

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Journal articles on the topic 'Alfven waves-Magnetized plasmas'

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