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Erkaev, N. V.
Solution for jump conditions at fast shocks in an anisotropic magnetized plasma / N. V. Erkaev, D. F. Vogl, H. K. Biernat // J. Plasma Phys. - 2000. - Vol. 64. - P. 561-578, DOI 10.1017/S002237780000893X. - Cited References: 10 . - ISSN 0022-3778

РУБ Physics, Fluids & Plasmas
Рубрики:
MAGNETOSHEATH
Кл.слова (ненормированные):
Magnetic anisotropy -- Magnetic field effects -- Magnetohydrodynamics -- Plasma sheaths -- Plasma shock waves -- Plasma stability -- Pressure effects -- Thermal effects -- Alfven Mach number -- Anisotropic magnetized plasma -- Jump condition -- Magnetoplasma
Аннотация: We study the magnetic field and plasma parameters downstream of a fast shock as functions of normalized upstream parameters and the rate of pressure anisotropy (defined as the ratio of perpendicular to parallel pressure). We analyse two cases: with the shock (i) perpendicular and (ii) inclined with respect to the magnetic field. The relations on the fast, shock in a magnetized anisotropic plasma are solved taking into account the criteria for the mirror instability and firehose instability bounding the pressure anisotropy downstream of the shock. Our analysis shows that the parallel pressure and the parallel temperature as well as the tangential component of the velocity are the parameters that are most sensitive to the rate of pressure anisotropy. The variations of the other parameters, namely density, normal velocity, tangential component of the magnetic field, perpendicular pressure, and perpendicular temperature are much less pronounced, in particular when the perpendicular pressure exceeds the parallel pressure. The variations of all parameters increase substantially for a very low rate of anisotropy, which is bounded by the firehose instability in the case of inclined shocks. Using the criterion for mirror instability as a closure relation for the jump conditions at the fast shock, we obtain the plasma parameters and the magnetic field downstream of the shock as functions of the Alfven Mach number. For each Alfven Mach number, the criterion for mirror instability determines the minimum jumps in such parameters as density, tangential magnetic field component, parallel pressure, and temperature. and determines the maximum values of the velocity components and the perpendicular temperature. Ideal anisotropic magnetohydrodynamics (MHD) has wide applications for space plasma physics. Observations of the field and plasma behaviour in the solar wind as well as in the Earth's magnetosheath have highlighted the need for an MHD model where the plasma pressure is treated as a tensor.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
Graz Univ, Inst Geophys, A-8010 Graz, Austria
Graz Univ, Inst Theoret Phys, A-8010 Graz, Austria
ИВМ СО РАН
Institute of Computational Modelling, Russian Academy of Sciences, Krasnoyarsk 660036, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Schmiedlstra?e 6, A-8042 Graz, Austria
Institute for Geophysics, Astrophysics, and Meteorology, University of Graz, Universitatsplatz 5, 8010 Graz, Austria
Institute for Theoretical Physics, University of Graz, Universitatsplatz 5, 8010 Graz, Austria

Доп.точки доступа:
Vogl, D. F.; Biernat, H. K.; Еркаев, Николай Васильевич
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Erkaev, N. V.
Ideal magnetohydrodynamic flow around a blunt body under anisotropic pressure / N. V. Erkaev, H. K. Biernat, C. J. Farrugia // Phys. Plasmas. - 2000. - Vol. 7, Is. 8. - P. 3413-3420, DOI 10.1063/1.874205. - Cited References: 23 . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
MHD FLOW
   MAGNETOSHEATH
   DEPLETION
   CLOSURE
   FLUID
   MODEL
Аннотация: The plasma flow past a blunt obstacle in an ideal magnetohydrodynamic (MHD) model is studied, taking into account the tensorial nature of the plasma pressure. Three different closure relations are explored and compared with one another. The first one is the adiabatic model proposed by Chew, Goldberger, and Low. The second closure is based on the mirror instability criterion, while the third depends on an empirical closure equation obtained from observations of solar wind flow past the Earth's magnetosphere. The latter is related with the criterion of the anisotropic ion cyclotron instability. In the presented model, the total pressure, defined as the sum of magnetic pressure and perpendicular plasma pressure, is assumed to be a known function of Cartesian coordinates. The calculation is based on the Newtonian approximation for the total pressure along the obstacle and on a quadratic behavior with distance from the obstacle along the normal direction. Profiles of magnetic field strength and plasma parameters are presented along the stagnation stream line between the shock and obstacle of an ideal plasma flow with anisotropy in thermal pressure and temperature. (C) 2000 American Institute of Physics. [S1070- 664X(00)04407-4].

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA
ИВМ СО РАН

Доп.точки доступа:
Biernat, H. K.; Farrugia, C. J.; Еркаев, Николай Васильевич
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Erkaev, N. V.
Reconnection rate for the inhomogeneous resistivity Petschek model / N. V. Erkaev, V. S. Semenov, F. . Jamitzky // Phys. Rev. Lett. - 2000. - Vol. 84, Is. 7. - P. 1455-1458, DOI 10.1103/PhysRevLett.84.1455. - Cited References: 16 . - ISSN 0031-9007

РУБ Physics, Multidisciplinary
Рубрики:
MAGNETIC RECONNECTION
CURRENT SHEETS
Аннотация: The reconnection rate for the canonical simplest case of steady-state two-dimensional symmetric reconnection in an incompressible plasma is found by matching of an outer Petschek solution and an internal diffusion region solution. The reconnection rate obtained naturally incorporates both Sweet-Parker and Petschek regimes; while the latter is possible only for a strongly localized resistivity.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
St Petersburg State Univ, Inst Phys, St Petersburg 198904, Russia
Max Planck Inst Extraterr Phys, D-85740 Garching, Germany
ИВМ СО РАН

Доп.точки доступа:
Semenov, V. S.; Jamitzky, F.; Еркаев, Николай Васильевич
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Rate of steady-state reconnection in an incompressible plasma / N. V. Erkaev [et al.] // Phys. Plasmas. - 2001. - Vol. 8, Is. 11. - P. 4800-4809, DOI 10.1063/1.1410112. - Cited References: 16 . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
MAGNETIC RECONNECTION
CURRENT SHEETS
MODEL
Аннотация: The reconnection rate is obtained for the simplest case of two-dimensional (2D) symmetric reconnection in an incompressible plasma. In the short note [Erkaev , Phys. Rev. Lett. 84, 1455 (2000)], the reconnection rate is found by matching the outer Petschek solution and the inner diffusion region solution. Here the details of the numerical simulation of the diffusion region are presented and the asymptotic procedure which is used for deriving the reconnection rate is described. The reconnection rate is obtained as a decreasing function of the diffusion region length. For a sufficiently large diffusion region scale, the reconnection rate becomes close to that obtained in the Sweet-Parker solution with the inverse square root dependence on the magnetic Reynolds number Re-m, determined for the global size of the current sheet. On the other hand, for a small diffusion region length scale, the reconnection rate turns out to be very similar to that obtained in the Petschek model with a logarithmic dependence on the magnetic Reynolds number Re-m. This means that the Petschek regime seems to be possible only in the case of a strongly localized conductivity corresponding to a small scale of the diffusion region. (C) 2001 American Institute of Physics.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036 36, Russia
Univ St Petersburg, Inst Phys, St Petersburg 198504, Russia
Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
ИВМ СО РАН
Institute of Computational Modelling, Russian Academy of Sciences, 660036 Krasnoyarsk 36, Russian Federation
Institute of Physics, University of St. Petersburg, St. Petergof 198504, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria

Доп.точки доступа:
Erkaev, N. V.; Еркаев, Николай Васильевич; Semenov, V. S.; Alexeev, I. V.; Biernat, H. K.
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Arshukova, I. L.
Magnetohydrodynamic instability of a high magnetic shear layer with a finite curvature radius / I. L. Arshukova, N. V. Erkaev, H. K. Biernat // Phys. Plasmas. - 2002. - Vol. 9, Is. 2. - P. 401-408, DOI 10.1063/1.1432698. - Cited References: 15 . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
KELVIN-HELMHOLTZ INSTABILITY
CURRENT SHEETS
Аннотация: This article deals with the magnetohydrodynamic instability of a thin layer which is characterized by a high magnetic shear, a constant curvature radius, and a plasma velocity shear. The magnetic field and the plasma parameters are considered to be piecewise constant inside the layer and in the regions adjacent to the layer. The plasma parameters and the magnetic field are assumed to obey the ideal incompressible magnetohydrodynamics. Fourier analysis is used to calculate small perturbations of the magnetic field and plasma parameters near the layer in linear approximation. The instability growth rate is obtained as a function of different parameters: the magnetic shear angle, the velocity direction angle, the tangential plasma velocity, the layer thickness, the wave number, and the curvature radius. The resulting instability is a mixture of interchange and Kelvin-Helmholtz instabilities on a surface with nonzero curvature. For a fixed velocity shear and curvature radius, the instability growth has a maximum in the case of antiparallel magnetic fields (maximal magnetic shear). This growth rate is an increasing function of the tangential velocity component perpendicular to the magnetic field, and a decreasing function of the velocity component along the magnetic field. The instability is stronger for smaller curvature radius. (C) 2002 American Institute of Physics.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
ИВМ СО РАН
Institute of Computational Modelling, Russian Academy of Sciences, Krasnoyarsk 660036, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria

Доп.точки доступа:
Erkaev, N. V.; Еркаев, Николай Васильевич; Biernat, H. K.
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Peculiarities of Alfven wave propagation along a nonuniform magnetic flux tube / N. V. Erkaev [et al.] // Phys. Plasmas. - 2005. - Vol. 12, Is. 1. - Ст. 12905, DOI 10.1063/1.1833392. - Cited References: 18 . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
HYDROMAGNETIC-WAVES
   TRANSFER EVENTS
   FIELD
   SLOW
Кл.слова (ненормированные):
Algebra -- Approximation theory -- Boundary conditions -- Electric conductivity -- Electric field effects -- Integral equations -- Magnetic flux -- Magnetohydrodynamics -- Perturbation techniques -- Polarization -- Vectors -- Velocity measurement -- Alfven wave propagation -- Axial symmetry -- Magnetic flux tubes -- Magnetosonic pulses -- Wave propagation
Аннотация: Within the framework of the assumption of large azimuthal wave numbers, the equations for Alfven and slow magnetosonic waves are obtained using frozen-in material coordinates. These equations are specified for the case of a nonuniform magnetic field with axial symmetry. Assuming a meridional polarization of the magnetic field and velocity perturbations, the effects of Alfven wave propagation are analyzed which are related to geometric characteristics of a nonuniform magnetic field: (a) A finite curvature radius of the magnetic field lines and (b) convergence of magnetic field lines. The interaction between the Alfven and magnetosonic waves is found to be strongly dependent on the curvature radius of the magnetic tube and the local plasma beta parameter. The electric field amplitude and the length scale of a wave front are found to increase very strongly in the course of the Alfven wave propagation along a converging magnetic flux tube. Also studied is a temporal decrease of the wave perturbations which is caused by dissipation at the conducting boundary. (C) 2005 American Institute of Physics.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
Krasnoyarsk State Univ, Krasnoyarsk 660041, Russia
St Petersburg State Univ, Inst Phys, St Petersburg 198504, Russia
Austrian Acad Sci, Inst Space Res, A-8042 Graz, Austria
ИВМ СО РАН
Intitute of Computational Modelling, Russian Academy of Sciences, Krasnoyarsk 660036, Russian Federation
State University of Krasnoyarsk, Krasnoyarsk 660041, Russian Federation
Institute of Physics, State University, St. Petersburg 198504, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria

Доп.точки доступа:
Erkaev, N. V.; Еркаев, Николай Васильевич; Shaidurov, V. A.; Semenov, V. S.; Langmayr, D.; Biernat, H. K.
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Langmayr, D.
Influence of kappa-distributed ions on the two-stream instability / D. . Langmayr, H. K. Biernat, N. V. Erkaev // Phys. Plasmas. - 2005. - Vol. 12, Is. 10. - Ст. 102103, DOI 10.1063/1.2065370. - Cited References: 30 . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
QUASI-PERPENDICULAR SHOCKS
   FIELD STREAMING INSTABILITY
   DISPERSION FUNCTION
   MIRROR INSTABILITY
   SPACE PLASMAS
   EQUILIBRIUM
Кл.слова (ненормированные):
Electromagnetic wave propagation -- Electrostatics -- Magnetism -- Magnetization -- Growth rate -- Modified two-stream instability (MTSI) -- Two-stream instability -- Plasma stability
Аннотация: This paper is the first approach for analyzing the influence of kappa-distributed particles on the modified two-stream instability (MTSI). It is assumed that the plasma consists of a magnetized Maxwellian electron contribution and unmagnetized kappa-distributed ions drifting across the electrons. Within an electrostatic approximation, the influence of the kappa parameter on the maximum growth rate of the MTSI is evaluated for the special case of parallel drift velocity and wave propagation.

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Держатели документа:
Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036, Russia
ИВМ СО РАН
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria
Institute of Computational Modelling, Russian Academy of Sciences, Krasnoyarsk 660036, Russian Federation

Доп.точки доступа:
Biernat, H. K.; Erkaev, N. V.; Еркаев, Николай Васильевич
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Erkaev, N. V.
Magnetic double-gradient instability and flapping waves in a current sheet / N. V. Erkaev, V. S. Semenov, H. K. Biernat // Phys. Rev. Lett. - 2007. - Vol. 99, Is. 23. - Ст. 235003, DOI 10.1103/PhysRevLett.99.235003. - Cited References: 10 . - ISSN 0031-9007

РУБ Physics, Multidisciplinary
Рубрики:
MAGNETOTAIL CURRENT SHEET
CLUSTER
Кл.слова (ненормированные):
Magnetic fields -- Magnetic properties -- Magnetohydrodynamics -- Velocity measurement -- Current sheets -- Flapping waves -- Magnetic gradients -- Stable regions -- Electromagnetic waves
Аннотация: A new kind of magnetohydrodynamic instability and waves are analyzed for a current sheet in the presence of a small normal magnetic field component varying along the sheet. These waves and instability are related to the existence of two gradients of the tangential (B(tau)) and normal (B(n)) magnetic field components along the normal (del(n)B(tau)) and tangential (del(tau)B(n)) directions with respect to the current sheet. The current sheet can be stable or unstable if the multiplication of two magnetic gradients is positive or negative. In the stable region, the kinklike wave mode is interpreted as so-called flapping waves observed in Earth's magnetotail current sheet. The kink wave group velocity estimated for the Earth's current sheet is of the order of a few tens of kilometers per second. This is in good agreement with the observations of the flapping motions of the magnetotail current sheet.

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Держатели документа:
Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk, Russia
Siberian Fed Univ, Krasnoyarsk, Russia
St Petersburg State Univ, Inst Phys, St Petersburg, Russia
Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria
Graz Univ, Inst Phys, Graz, Austria
ИВМ СО РАН
Institute of Computational Modelling, Russian Academy of Sciences, Krasnoyarsk, Russian Federation
Siberian Federal University, Krasnoyarsk, Russian Federation
Institute of Physics, State University of St. Petersburg, St. Petersburg, Russian Federation
Space Research Institute, Austrian Academy of Sciences, Graz, Austria
Institute of Physics, University of Graz, Graz, Austria

Доп.точки доступа:
Semenov, V. S.; Biernat, H. K.; Еркаев, Николай Васильевич
}
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Shear driven waves in the induced magnetosphere of Mars / H. . Gunell [et al.] // Plasma Phys. Control. Fusion. - 2008. - Vol. 50, Is. 7. - Ст. 74018, DOI 10.1088/0741-3335/50/7/074018. - Cited References: 27 . - ISSN 0741-3335

РУБ Physics, Fluids & Plasmas + Physics, Nuclear
Рубрики:
SOLAR-WIND INTERACTION
   KELVIN-HELMHOLTZ INSTABILITY
   MARTIAN ATMOSPHERE
   VELOCITY SHEAR
   VENUS
   PLASMA
   MHD
   IONOPAUSE
   SIMULATIONS
   BOUNDARY
Кл.слова (ненормированные):
Charged particles -- Magnetosphere -- Motion estimation -- Natural frequencies -- Plasma stability -- Shearing machines -- p ,p ,t measurements -- Computational results -- Electron densities -- Fundamental frequency (FF) -- Higher harmonics -- ion densities -- Ion velocities -- velocity shear -- Electrons
Аннотация: We present measurements of oscillations in the electron density, ion density and ion velocity in the induced magnetosphere of Mars. The fundamental frequency of the oscillations is a few millihertz, but higher harmonics are present in the spectrum. The oscillations are observed in a region where there is a velocity shear in the plasma flow. The fundamental frequency is in agreement with computational results from an ideal-MHD model. An interpretation based on velocity-shear instabilities is described.

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Держатели документа:
[Gunell, H.
Koepke, M.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA
[Amerstorfer, U. V.
Biernat, H. K.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
[Amerstorfer, U. V.
Biernat, H. K.] Graz Univ, Inst Phys, A-8010 Graz, Austria
[Nilsson, H.
Holmstrom, M.
Lundin, R.
Barabash, S.] Swedish Inst Space Phys, SE-98128 Kiruna, Sweden
[Grima, C.] Lab Planetol Grenoble, F-38041 Grenoble 9, France
[Fraenz, M.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany
[Winningham, J. D.
Frahm, R. A.] SW Res Inst, San Antonio, TX USA
[Sauvaud, J-A
Fedorov, A.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France
[Erkaev, N. V.] Russian Acad Sci, Inst Computat Modelling, Krasnoyarsk 660036 36, Russia
ИВМ СО РАН
Department of Physics, West Virginia University, Morgantown, WV 26506-6315, United States
Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, A-8042 Graz, Austria
Institute of Physics, University of Graz, Universitatsplatz 5, A-8010 Graz, Austria
Swedish Institute of Space Physics, P.O. Box812, SE-981 28 Kiruna, Sweden
Laboratoire de Planetologie de Grenoble, BP-53, F-38041 Grenoble Cedex 9, France
Max-Planck-Institut fur Sonnensystemforschung, Max-Planck-Stra?e 2, 37191 Katlenburg-Lindau, Germany
Southwest Research Institute, San Antonio, TX 7228-0510, United States
Centre d'Etude Spatiale des Rayonnements, BP-4346, F-31028 Toulouse, France
Institute of Computational Modelling, Russian Academy of Sciences, 660036 Krasnoyarsk-36, Russian Federation

Доп.точки доступа:
Gunell, H.; Amerstorfer, U. V.; Nilsson, H.; Grima, C.; Koepke, M.; Franz, M.; Winningham, J. D.; Frahm, R. A.; Sauvaud, J. A.; Fedorov, A.; Erkaev, N. V.; Еркаев, Николай Васильевич; Biernat, H. K.; Holmstrom, M.; Lundin, R.; Barabash, S.
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10.

Kinetic Alfven wave instability in a Lorentzian dusty magnetoplasma / N. . Rubab [et al.] // Phys. Plasmas. - 2010. - Vol. 17, Is. 10. - Ст. 103704, DOI 10.1063/1.3491336. - Cited References: 54. - This work is funded by the Higher Education Commission of Pakistan under the HEC-Overseas scholarship program Grant No. Ref: 1-1/PM OS /Phase-II/Batch-I/Austria/2007/. Part of this work was done while N. V. Erkaev was at the Space Research Institute of the Austrian Academy of Sciences in Graz. This work is also supported due to the RFBR Grant No. 09-05-91000-ANF-a. Further support is due to the "Austrian Fonds zur Forderung der Wissenschaftlichen Forschung" under Grant No. P20145-N16. . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
MAXWELLIAN DISTRIBUTION-FUNCTIONS
   FREQUENCY ELECTROMAGNETIC-WAVES
   SOLAR-WIND
   CHARGE FLUCTUATION
   2-STREAM INSTABILITIES
   ELECTROSTATIC MODES
   SPACE PLASMAS
   ION PLASMA
   TEMPERATURE
   PROPAGATION
Кл.слова (ненормированные):
Analytical expressions -- Dispersion relations -- Distributed streaming -- Dust acoustic -- Dust particle -- Growth rate of instabilities -- Magnetized electrons -- N-waves -- Potential theory -- Slow motion -- Streaming velocity -- Theoretical approach -- Two stream instability -- Whistler waves -- Dust -- Magnetic field effects -- Plasma waves -- Stability -- Acoustic wave propagation
Аннотация: This study presents a theoretical approach to analyze the influence of kappa distributed streaming ions and magnetized electrons on the plasma wave propagation in the presence of dust by employing two-potential theory. In particular, analytical expressions under certain conditions are derived for various modes of propagation comprising of kinetic Alfven wave streaming instability, two stream instability, and dust acoustic and whistler waves. A dispersion relation for kinetic Alfven-like streaming instability has been derived. The effects of dust particles and Lorentzian index on the growth rates and the threshold streaming velocity for the excitation of the instability are examined. The streaming velocity is observed to be destabilizing for slow motion and stabilizing for fast streaming motions. It is also observed that the presence of magnetic field and superthermal particles hinders the growth rate of instability. Possible applications to various space and astrophysical situations are discussed. (C) 2010 American Institute of Physics. [doi:10.1063/1.3491336]

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Держатели документа:
[Rubab, N.
Biernat, H. K.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
[Rubab, N.
Biernat, H. K.] Graz Univ, Inst Phys, A-8010 Graz, Austria
[Erkaev, N. V.] Inst Computat Modelling, Krasnoyarsk 660036, Russia
[Erkaev, N. V.] Siberian Fed Univ, Krasnoyarsk 660041, Russia
[Langmayr, D.] Virtual Vehicle Competence Ctr Vif, A-8010 Graz, Austria
ИВМ СО РАН
Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria
And Institute of Physics, University of Graz, Universitatplatz 5, A-8010 Graz, Austria
Institute of Computational Modelling, 660036 Krasnoyarsk, Russian Federation
Siberian Federal University, 660041 Krasnoyarsk, Russian Federation
Virtual Vehicle Competence Center (Vif), Inffeldgasse 21a, 8010 Graz, Austria

Доп.точки доступа:
Rubab, N.; Erkaev, N. V.; Еркаев, Николай Васильевич; Langmayr, D.; Biernat, H. K.
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