Log in

Relevant bibliographies by topics / Plasma turbulence theory / Journal articles

To see the other types of publications on this topic, follow the link: Plasma turbulence theory.

Journal articles on the topic 'Plasma turbulence theory'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the top 50 journal articles for your research on the topic 'Plasma turbulence theory.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Browse journal articles on a wide variety of disciplines and organise your bibliography correctly.

1

Tong, Y., and A. C. L. Chian. "Dynamo Driven by Weak Plasma Turbulence." Symposium - International Astronomical Union 157 (1993): 249–50. http://dx.doi.org/10.1017/s0074180900174212.

Full text

Abstract:

We discuss a dynamo mechanism driven by weak plasma turbulence and show that turbulent plasma waves may generate and maintain cosmic magnetic field. A dynamo equation is derived from the magnetic induction equation based on mean field electrodynamics. In the usual α–ω dynamo theory, the source term in the dynamo equation arises from α–effect associated with the convective motion of the fluid. In contrast, in our theory the source term is determined by “P–effcct” associated with weakly turbulent waves (e.g. Alfvén waves) in the plasma. We suggest that “P–ω” dynamo may be operative either in the presence or absence of convection. The sole requirement for its operation is the existence of weak plasma turbulence in the source region of the cosmic magnetic field.

APA, Harvard, Vancouver, ISO, and other styles

2

Ishihara, Osamu, Huajuan Xia, and Akira Hirose. "Resonance broadening theory of plasma turbulence." Physics of Fluids B: Plasma Physics 4, no. 2 (February 1992): 349–62. http://dx.doi.org/10.1063/1.860283.

Full text

APA, Harvard, Vancouver, ISO, and other styles

3

Schlickeiser, Reinhard, and Ulrich Achatz. "Cosmic-ray particle transport in weakly turbulent plasmas. Part 1. Theory." Journal of Plasma Physics 49, no. 1 (February 1993): 63–77. http://dx.doi.org/10.1017/s0022377800016822.

Full text

Abstract:

We consider a quasi-linear theory for the acceleration rates and propagation parameters of charged test particles in weakly turbulent electromagnetic plasmas. The similarity between two recent approaches to modelling of therandom electromagnetic field is demonstrated. It is shown that both the concept of dynamical magnetic turbulence and the concept of superposition of individual plasma modes lead to particle Fokker—Planck coefficients in which the sharp delta functions describing the resonant interaction of the particles have to be replaced by Breit—Wigner-type resonance functions, which are controlled by the dynamical turbulence decay time and the wave-damping time respectively. The resulting resonance broadening will significantly change the evaluation of cosmic-ray transport parameters.

APA, Harvard, Vancouver, ISO, and other styles

4

Terry, P. W. "Theory of critical balance in plasma turbulence." Physics of Plasmas 25, no. 9 (September 2018): 092301. http://dx.doi.org/10.1063/1.5041754.

Full text

APA, Harvard, Vancouver, ISO, and other styles

5

Yoshizawa, A., S. I. Itoh, and K. Itoh. "Plasma and Fluid Turbulence: Theory and Modelling." Plasma Physics and Controlled Fusion 45, no. 3 (February 24, 2003): 321–22. http://dx.doi.org/10.1088/0741-3335/45/3/701.

Full text

APA, Harvard, Vancouver, ISO, and other styles

6

De Angelis, Elisabetta. "Plasma and Fluid Turbulence: Theory and Modelling." Applied Rheology 13, no. 2 (April 1, 2003): 69. http://dx.doi.org/10.1515/arh-2003-0024.

Full text

APA, Harvard, Vancouver, ISO, and other styles

7

Yoon, Peter H. "Weak turbulence theory for beam-plasma interaction." Physics of Plasmas 25, no. 1 (January 2018): 011603. http://dx.doi.org/10.1063/1.5017518.

Full text

APA, Harvard, Vancouver, ISO, and other styles

8

Rönnmark, K., and T. Biro. "Phase-space description of plasma waves. Part 2. Nonlinear theory." Journal of Plasma Physics 47, no. 3 (June 1992): 479–89. http://dx.doi.org/10.1017/s0022377800024363.

Full text

Abstract:

A representation of the physical fields as functions on (k, ω, r, t) phase space can be based on Gaussian windows and Fourier transforms. Within this representation, we obtain a very general formula for the second-order nonlinear current J(k, ω, r, t) in terms of the vector potential A(k, ω, r, t). This formula is a convenient starting point for studies of coherent as well as turbulent nonlinear processes. We derive kinetic equations for weakly inhomogeneous and turbulent plasmas, including the effects of inhomogeneous turbulence, wave convection and refraction.

APA, Harvard, Vancouver, ISO, and other styles

9

Mel’nik, Valentin. "Plasma Theory of Solar Radar Echoes after Thirty Years." Highlights of Astronomy 12 (2002): 389. http://dx.doi.org/10.1017/s1539299600013836.

Full text

Abstract:

In 1967 Gordon made the revolutionary assumption that reflection of radar signal from the Sun can be explained by its scattering on microturbulence (Gordon 1973). In his first model it was ion-sound turbulence. Later he considered radar scattering on Langmuir turbulence. The principal opportunity to explain frequency displacements of radar echoes observed in James’ experiments (James 1966, 1970) was shown. However, it turned out (Gerasimova 1979) that the mechanism needed an impermissible high level of isotropic turbulence for the reflection with cross-sectionsσ= 10πR2ʘ.

APA, Harvard, Vancouver, ISO, and other styles

10

Zhou, Ye. "Renormalization group theory for fluid and plasma turbulence." Physics Reports 488, no. 1 (March 2010): 1–49. http://dx.doi.org/10.1016/j.physrep.2009.04.004.

Full text

APA, Harvard, Vancouver, ISO, and other styles

11

Wang, Shaojie. "Lie-transform theory of transport in plasma turbulence." Physics of Plasmas 21, no. 7 (July 2014): 072312. http://dx.doi.org/10.1063/1.4890356.

Full text

APA, Harvard, Vancouver, ISO, and other styles

12

Hanssen, Alfred. "Resonance broadening modification of weak plasma turbulence theory." Journal of Geophysical Research: Space Physics 96, A2 (February 1, 1991): 1867–71. http://dx.doi.org/10.1029/90ja02307.

Full text

APA, Harvard, Vancouver, ISO, and other styles

13

Hamabata, Hiromitsu. "Modulational instability produced by Alfvénic turbulence in a collisionless plasma." Journal of Plasma Physics 46, no. 2 (October 1991): 319–30. http://dx.doi.org/10.1017/s0022377800016147.

Full text

Abstract:

Using first-order smoothing theory, Fourier analysis and perturbation methods, we obtain the evolution equation of the wave spectrum as well as the nonlinear forces generated by Alfvénic turbulence in a finite-β plasma with dispersion and phenomenological Landau-damping effects. The stability of Alfvénic turbulence is then analysed by solving the derived mean-field equations. It is shown that parallel-propagating turbulent Alfvén waves with dispersion can be modulationally unstable, leading to amplification of large-scale Alfvén waves and acoustic waves when Landau-damping effects are strong and weak respectively.

APA, Harvard, Vancouver, ISO, and other styles

14

Yoshizawa,, A., S.-I. Itoh ,, K. Itoh,, and Toshi Tajima,. "Plasma and Fluid Turbulence: Theory and Modelling. Series in Plasma Physics." Applied Mechanics Reviews 57, no. 1 (January 1, 2004): B5—B6. http://dx.doi.org/10.1115/1.1641779.

Full text

APA, Harvard, Vancouver, ISO, and other styles

15

Erofeev, V. I. "Weak Plasma Turbulence Theory and Some Other Items of Plasma Kinetics." Australian Journal of Physics 51, no. 5 (1998): 843. http://dx.doi.org/10.1071/p97080.

Full text

Abstract:

A new approach to a plasma kinetic description is discussed, the beginnings of which were published recently (Erofeev 1997a). It is shown that calculations of the three-wave collision integral following this approach confirm the intensity and structure of the three-wave collision integral obtained in the traditional theory. The reported kinetics extend the area of applicability for the weak plasma turbulence theory: apart from waves it properly accounts for the effect of various other plasma nonlinear structures of the type of solitons, drift vortices, collapsing cavities and so on. Some directions for further studies are also discussed.

APA, Harvard, Vancouver, ISO, and other styles

16

Keskinen, M. J. "Theory of Strongly Turbulent Two-Dimensional Cross Field Convection of Current Carrying Space Plasmas." Symposium - International Astronomical Union 107 (1985): 475. http://dx.doi.org/10.1017/s0074180900075963.

Full text

Abstract:

The “direct interaction approximation” of Kraichnan as modified by Kadomtsev is employed to develop a two-dimensional strong turbulence theory which predicts both nonlinear frequency broadening and a power law for the spectrum of a convecting plasma containing a gravitationally induced cross field current. These results are favorably compared with experimental observations, numerical simulations, and previous studies1 of turbulent cross field convection of current-carrying plasma.

APA, Harvard, Vancouver, ISO, and other styles

17

Shishov, V. I. "Interstellar Scintillation and Clouds of the Interstellar Turbulent Plasma." International Astronomical Union Colloquium 182 (2001): 163–69. http://dx.doi.org/10.1017/s0252921100000907.

Full text

Abstract:

AbstractData on interstellar diffraction and refraction scintillation of pulsars are analyzed. Comparison between theory and the observational data shows that two types of spectra for electron density fluctuations are realized in the interstellar medium: pure power law and piecewise with a break. The distribution of turbulent plasma in the Galaxy has a three component structure. Component A is diffuse and it is distributed outside of the spiral arms of the Galaxy. Component BI is cloudy and associated with Galactic arms. Component BII is extremely nonuniform and associated with HII regions and supernova remnants. The origin of the interstellar plasma turbulence is considered, and possible sources of turbulent energy are discussed. The contribution of supernova bursts in the interstellar gas ionization and generation of turbulence are analyzed among other factors.

APA, Harvard, Vancouver, ISO, and other styles

18

André, R., C. Hanuise, J. P. Villain, and V. Krasnoselskikh. "Turbulence characteristics inside ionospheric small-scale expanding structures observed with SuperDARN HF radars." Annales Geophysicae 21, no. 8 (August 31, 2003): 1839–45. http://dx.doi.org/10.5194/angeo-21-1839-2003.

Full text

Abstract:

Abstract. Unusual structures characterized by a very high-velocity divergence have been observed in the high-latitude F-region with SuperDARN radars (André et al., 2000). These structures have been interpreted as due to local demagnetization of the plasma in the ionospheric F-region, during very specific geophysical conditions. In this study, the collective wave scattering theory is used to characterize the decameter-scale turbulence (l approx 15 m) inside the structures. The distribution function of the diffusion coefficient is modified when the structures are generated, suggesting that two regimes of turbulence coexist. A temporal analysis decorrelates the two regimes and gives access to the dynamics associated with the structures. It is shown that a high turbulent regime precedes the plasma demagnetization and should be related to an energy deposition. Then a second regime appears when the plasma is demagnetized and disappears simultaneously with the structures. This study is the first application of the collective wave scattering theory to a specific geophysical event.Key words. Ionosphere (auroral ionosphere; ionospheric irregularities) – Space plasma physics (turbulence)

APA, Harvard, Vancouver, ISO, and other styles

19

Gibson, Carl H., and R. Norris Keeler. "The cosmic web and microwave background fossilize the first turbulent combustion." Proceedings of the International Astronomical Union 11, S308 (June 2014): 636–37. http://dx.doi.org/10.1017/s1743921316010747.

Full text

Abstract:

AbstractCollisional fluid mechanics theory predicts a turbulent hot big bang at Planck conditions from large, negative, turbulence stresses below the Fortov-Kerr limit (< −10113Pa). Big bang turbulence fossilized when quarks formed, extracting the mass energy of the universe by extreme negative viscous stresses of inflation, expanding to length scales larger than the horizon scale ct. Viscous-gravitational structure formation by fragmentation was triggered at big bang fossil vorticity turbulence vortex lines during the plasma epoch, as observed by the Planck space telescope. A cosmic web of protogalaxies, protogalaxyclusters, and protogalaxysuperclusters that formed in turbulent boundary layers of the spinning voids are hereby identified as expanding turbulence fossils that falsify CDMHC cosmology.

APA, Harvard, Vancouver, ISO, and other styles

20

Lazarian, A., G. Eyink, E. Vishniac, and G. Kowal. "Turbulent reconnection and its implications." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 373, no. 2041 (May 13, 2015): 20140144. http://dx.doi.org/10.1098/rsta.2014.0144.

Full text

Abstract:

Magnetic reconnection is a process of magnetic field topology change, which is one of the most fundamental processes happening in magnetized plasmas. In most astrophysical environments, the Reynolds numbers corresponding to plasma flows are large and therefore the transition to turbulence is inevitable. This turbulence, which can be pre-existing or driven by magnetic reconnection itself, must be taken into account for any theory of magnetic reconnection that attempts to describe the process in the aforementioned environments. This necessity is obvious as three-dimensional high-resolution numerical simulations show the transition to the turbulence state of initially laminar reconnecting magnetic fields. We discuss ideas of how turbulence can modify reconnection with the focus on the Lazarian & Vishniac (Lazarian & Vishniac 1999 Astrophys. J. 517, 700–718 ()) reconnection model. We present numerical evidence supporting the model and demonstrate that it is closely connected to the experimentally proven concept of Richardson dispersion/diffusion as well as to more recent advances in understanding of the Lagrangian dynamics of magnetized fluids. We point out that the generalized Ohm's law that accounts for turbulent motion predicts the subdominance of the microphysical plasma effects for reconnection for realistically turbulent media. We show that one of the most dramatic consequences of turbulence is the violation of the generally accepted notion of magnetic flux freezing. This notion is a cornerstone of most theories dealing with magnetized plasmas, and therefore its change induces fundamental shifts in accepted paradigms, for instance, turbulent reconnection entails reconnection diffusion process that is essential for understanding star formation. We argue that at sufficiently high Reynolds numbers the process of tearing reconnection should transfer to turbulent reconnection. We discuss flares that are predicted by turbulent reconnection and relate this process to solar flares and γ-ray bursts. With reference to experiments, we analyse solar observations in situ as measurements in the solar wind or heliospheric current sheet and show the correspondence of data with turbulent reconnection predictions. Finally, we discuss first-order Fermi acceleration of particles that is a natural consequence of the turbulent reconnection.

APA, Harvard, Vancouver, ISO, and other styles

21

Sarma, S. N., K. K. Sarma, and M. Nambu. "Plasma maser theory of the extraordinary mode in the presence of Langmuir turbulence." Journal of Plasma Physics 46, no. 2 (October 1991): 331–46. http://dx.doi.org/10.1017/s0022377800016159.

Full text

Abstract:

The emission of extraordinary mode radiation in a plasma with Langmuir turbulence driven by an electron beam is considered. The process of emission considered in this paper is the plasma maser effect, which is essentially an energy up-conversion process. The energy necessary for the growth of the extraordinary mode is derived from the Langmuir turbulence. The nonlinear dispersion relation of the extraordinary mode in the presence of Langmuir turbulence is obtained and its growth rate calculated. The scope of application of the results to space-plasma observation is then stressed.

APA, Harvard, Vancouver, ISO, and other styles

22

Materassi, M., and G. Consolini. "Turning the resistive MHD into a stochastic field theory." Nonlinear Processes in Geophysics 15, no. 4 (August 27, 2008): 701–9. http://dx.doi.org/10.5194/npg-15-701-2008.

Full text

Abstract:

Abstract. Classical systems stirred by random forces of given statistics may be described via a path integral formulation in which their degrees of freedom are stochastic variables themselves, undergoing a multiple-history probabilistic evolution. This framework seems to be easily applicable to resistive Magneto-Hydro-Dynamics (MHD). Indeed, MHD equations form a dynamic system of classical variables in which the terms representing the density, the pressure and the conductivity of the plasma are irregular functions of space and time when turbulence occurs. By treating those irregular terms as random stirring forces, it is possible to introduce a Stochastic Field Theory which should represent correctly the impulsive phenomena caused by the spece- and time-irregularity of plasma turbulence. This work is motivated by the recent observational evidences of the crucial role played by stochastic fluctuations in space plasmas.

APA, Harvard, Vancouver, ISO, and other styles

23

Mikhailenko, V. S., V. V. Mikhailenko, and K. N. Stepanov. "Renormalized theory of drift turbulence in plasma shear flows." Plasma Physics and Controlled Fusion 52, no. 5 (March 31, 2010): 055007. http://dx.doi.org/10.1088/0741-3335/52/5/055007.

Full text

APA, Harvard, Vancouver, ISO, and other styles

24

Spanier, Felix, and Rami Vainio. "Weak turbulence theory of dispersive waves in the solar corona." Proceedings of the International Astronomical Union 6, S274 (September 2010): 133–36. http://dx.doi.org/10.1017/s1743921311006739.

Full text

Abstract:

AbstractThe interaction of plasma waves plays a crucial role in the dynamics of weakly turbulent plasmas. So far the interaction of non-dispersive waves has been studied. In this paper the theory is extended to dispersive waves. It is well known that dispersive waves may be found in the solar corona, where they contribute to the heating of the corona. Here the possible interactions in the solar corona are described and the interaction rates are derived in the framework of Hall MHD.

APA, Harvard, Vancouver, ISO, and other styles

25

Podesta, J. J. "Solar wind turbulence: Advances in observations and theory." Proceedings of the International Astronomical Union 6, S274 (September 2010): 295–301. http://dx.doi.org/10.1017/s1743921311007162.

Full text

Abstract:

AbstractObservations of plasma and magnetic field fluctuations in the solar wind provide a valuable source of information for the study of turbulence in collisionless astrophysical plasmas. Scientific data collected by various spacecraft over the last few decades has fueled steady progress in this field. Theoretical models, numerical simulations, and comparisons between theory and experiment have also contributed greatly to these advances. This review highlights some recent advances on the observational side including measurements of the anisotropy of inertial range fluctuations as revealed by the different scaling laws parallel and perpendicular to the mean magnetic field, measurements of the normalized cross-helicity spanning the entire inertial range which demonstrate that this quantity is scale invariant, and improved measurements of the spectrum of magnetic field fluctuations in the dissipation range that show a spectral break near the lengthscale of the electron gyro-radius. The theoretical implications of these results and comparisons between theory and observations are briefly summarized.

APA, Harvard, Vancouver, ISO, and other styles

26

Oughton, S., W. H. Matthaeus, M. Wan, and K. T. Osman. "Anisotropy in solar wind plasma turbulence." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 373, no. 2041 (May 13, 2015): 20140152. http://dx.doi.org/10.1098/rsta.2014.0152.

Full text

Abstract:

A review of spectral anisotropy and variance anisotropy for solar wind fluctuations is given, with the discussion covering inertial range and dissipation range scales. For the inertial range, theory, simulations and observations are more or less in accord, in that fluctuation energy is found to be primarily in modes with quasi-perpendicular wavevectors (relative to a suitably defined mean magnetic field), and also that most of the fluctuation energy is in the vector components transverse to the mean field. Energy transfer in the parallel direction and the energy levels in the parallel components are both relatively weak. In the dissipation range, observations indicate that variance anisotropy tends to decrease towards isotropic levels as the electron gyroradius is approached; spectral anisotropy results are mixed. Evidence for and against wave interpretations and turbulence interpretations of these features will be discussed. We also present new simulation results concerning evolution of variance anisotropy for different classes of initial conditions, each with typical background solar wind parameters.

APA, Harvard, Vancouver, ISO, and other styles

27

Boldyrev, Stanislav, Konstantinos Horaites, Qian Xia, and Jean Carlos Perez. "TOWARD A THEORY OF ASTROPHYSICAL PLASMA TURBULENCE AT SUBPROTON SCALES." Astrophysical Journal 777, no. 1 (October 15, 2013): 41. http://dx.doi.org/10.1088/0004-637x/777/1/41.

Full text

APA, Harvard, Vancouver, ISO, and other styles

28

Xiaogang, Wang, and Qiu Xiaoming (X M. Qhiu). "Theory of "clumps" in drift-wave turbulence in tokamak plasma." Chinese Physics Letters 3, no. 8 (August 1986): 377–79. http://dx.doi.org/10.1088/0256-307x/3/8/011.

Full text

APA, Harvard, Vancouver, ISO, and other styles

29

Krommes, J. A. "Recent results on analytical plasma turbulence theory: realizability, intermittency, submarginal turbulence and self-organized criticality." Plasma Physics and Controlled Fusion 41, no. 3A (January 1, 1999): A641—A652. http://dx.doi.org/10.1088/0741-3335/41/3a/058.

Full text

APA, Harvard, Vancouver, ISO, and other styles

30

Panchenko, V. G., and P. V. Porytsky. "Influence of Inhomogeneity on Transformation and Radiation Processes in Plasma with Upper Hybrid Pump." Ukrainian Journal of Physics 64, no. 9 (October 11, 2019): 814. http://dx.doi.org/10.15407/ujpe64.9.814.

Full text

Abstract:

On the basis of the kinetic theory of fluctuations, the processes of the longitudinal Langmuir wave transformation into a transverse electromagnetic wave in the turbulent inhomogeneous plasma have been studied. The plasma turbulence is assumed to arise owing to the parametric decay of the upper hybrid pump wave into a daughter wave and electron-drift oscillations. The transformation coefficient under the parametric instability saturation conditions is determined. The intensity of the electromagnetic radiation emission from the plasma is calculated, and its dependence on the plasma and pump wave parameters is found.

APA, Harvard, Vancouver, ISO, and other styles

31

Lominadze, J. G. "Development of the theory of instabilities of differentially rotating plasma with astrophysical applications." Proceedings of the International Astronomical Union 6, S274 (September 2010): 318–24. http://dx.doi.org/10.1017/s1743921311007216.

Full text

Abstract:

AbstractInstabilities of nonuniform flows is a fundamental problem in dynamics of fluids and plasmas. This presentation outlines atypical dynamics of instabilities for unmagnetized and magnetized astrophysical differentially rotating flows, including, our efforts in the development of general theory of magneto rotation instability (MRI) that takes into account plasma compressibility, pressure anisotropy, dissipative and kinetic effects. Presented analysis of instability (transient growth) processes in unmagnetized/hydrodynamic astrophysical disks is based on the breakthrough of the hydrodynamic community in the 1990s in the understanding of shear flow non-normality induced dynamics. This analysis strongly suggests that the so-called bypass concept of turbulence, which has been developed by the hydrodynamic community for spectrally stable shear flows, can also be applied to Keplerian disks. It is also concluded that the vertical stratification of the disks is an important ingredient of dynamical processes resulting onset of turbulence.

APA, Harvard, Vancouver, ISO, and other styles

32

Hora, Heinrich. "Hydrodynamic derivation of double layers (DL) and electric fields in plasmas." Laser and Particle Beams 3, no. 1 (February 1985): 59–78. http://dx.doi.org/10.1017/s0263034600001270.

Full text

Abstract:

The hitherto successful hydrodynamic plasma theory needed the simplifying assumption of quasi-neutrality. Earlier known ambipolar fields in plasma surfaces were considered as exceptions and Alfvén's model of a complementary description by plasma currents was criticized. Fields in plasmas were derived from the kinetic theory of turbulence. Following a model for the nonlinear force of laser–plasma interaction, we needed a general description of the plasma without space charge neutrality which succeeded numerically and analytically. High electric fields due to inhomogeneities inside plasmas were derived explaining for the first time quantitatively the reduction of thermal conduction in laser-fusion, the measured inverted double layers including a new type of resonance process, the MeV α-upshift by nonlinear-force driven caviton fields and the radial fields in tokamaks which cause plasma rotation.

APA, Harvard, Vancouver, ISO, and other styles

33

Melrose, D. B. "The Status of Pulsar Emission Theory." International Astronomical Union Colloquium 177 (2000): 721–26. http://dx.doi.org/10.1017/s0252921100061066.

Full text

Abstract:

AbstractIt is argued that there is now a preferred pulsar radio emission mechanism, involving beam-driven Langmuir turbulence. A testable prediction is that, at least in a statistical sense, features in the spectra of pulsars should scale with the plasma frequency,υGJ, implied by the Goldreich-Julian number density.

APA, Harvard, Vancouver, ISO, and other styles

34

ANDRUSHCHENKO, ZHANNA N., MARTIN JUCKER, and VLADIMIR P. PAVLENKO. "Self-consistent model of electron drift mode turbulence." Journal of Plasma Physics 74, no. 1 (February 2008): 21–33. http://dx.doi.org/10.1017/s0022377807006484.

Full text

Abstract:

AbstractThe nonlinear dynamics of magnetic electron drift mode turbulence are outlined and the generation of large-scale magnetic structures in a non-uniform magnetized plasma by turbulent Reynolds stress is demonstrated. The loop-back of large-scale flows on the microturbulence is elucidated and the modulation of the electron drift mode turbulence spectrum in a medium with slowly varying parameters is presented. The wave kinetic equation in the presence of large-scale flows is derived and it can be seen that the small-scale turbulence and the large-scale structures form a self-regulating system. Finally, it is shown by the use of quasilinear theory that the shearing of microturbulence by the flows can be described by a diffusion equation in k-space and the corresponding diffusion coefficients are calculated.

APA, Harvard, Vancouver, ISO, and other styles

35

ITOH, Kimitaka, Sanae-I. ITOH, Atsushi FUKUYAMA, and Masatoshi YAGI. "Theory of Plasma Turbulence and Structural Formation-Nonlinearity and Statistical View-." Journal of Plasma and Fusion Research 79, no. 6 (2003): 608–24. http://dx.doi.org/10.1585/jspf.79.608.

Full text

APA, Harvard, Vancouver, ISO, and other styles

36

Zhang, Y. Z., and S. M. Mahajan. "Correlation theory of a two‐dimensional plasma turbulence with shear flow." Physics of Fluids B: Plasma Physics 5, no. 7 (July 1993): 2000–2020. http://dx.doi.org/10.1063/1.860788.

Full text

APA, Harvard, Vancouver, ISO, and other styles

37

Silin, V. P. "Theory of ion-acoustic turbulence in plasma with anisotropically heated ions." Plasma Physics Reports 37, no. 5 (May 2011): 461–73. http://dx.doi.org/10.1134/s1063780x11050114.

Full text

APA, Harvard, Vancouver, ISO, and other styles

38

Kim, Y. B., P. H. Diamond, H. Biglari, and P. W. Terry. "Theory of resistivity‐gradient‐driven turbulence in a differentially rotating plasma." Physics of Fluids B: Plasma Physics 2, no. 9 (September 1990): 2143–50. http://dx.doi.org/10.1063/1.859434.

Full text

APA, Harvard, Vancouver, ISO, and other styles

39

Jovanović, Dušan, Olga Alexandrova, and Milan Maksimović. "Theory of coherent electron-scale magnetic structures in space plasma turbulence." Physica Scripta 90, no. 8 (June 10, 2015): 088002. http://dx.doi.org/10.1088/0031-8949/90/8/088002.

Full text

APA, Harvard, Vancouver, ISO, and other styles

40

Yi, Tong, Lu Shengzhi, Mao Xinjie, and Han Jiling. "The dynamo theory of plasma turbulence wave in rotating celestial bodies." Astrophysics and Space Science 113, no. 2 (1985): 303–16. http://dx.doi.org/10.1007/bf00650965.

Full text

APA, Harvard, Vancouver, ISO, and other styles

41

Santos-Lima, R., G. Guerrero, E. M. de Gouveia Dal Pino, and A. Lazarian. "Diffusion of large-scale magnetic fields by reconnection in MHD turbulence." Monthly Notices of the Royal Astronomical Society 503, no. 1 (February 18, 2021): 1290–309. http://dx.doi.org/10.1093/mnras/stab470.

Full text

Abstract:

ABSTRACT The rate of magnetic field diffusion plays an essential role in several astrophysical plasma processes. It has been demonstrated that the omnipresent turbulence in astrophysical media induces fast magnetic reconnection, which consequently leads to large-scale magnetic flux diffusion at a rate independent of the plasma microphysics. This process is called 'reconnection diffusion' (RD) and allows for the diffusion of fields, which are dynamically important. The current theory describing RD is based on incompressible magnetohydrodynamic (MHD) turbulence. In this work, we have tested quantitatively the predictions of the RD theory when magnetic forces are dominant in the turbulence dynamics (Alfvénic Mach number MA < 1). We employed the Pencil Code to perform numerical simulations of forced MHD turbulence, extracting the values of the diffusion coefficient ηRD using the test-field method. Our results are consistent with the RD theory ($\eta _{\rm RD} \sim M_{\rm A}^{3}$ for MA < 1) when turbulence approaches the incompressible limit (sonic Mach number MS ≲ 0.02), while for larger MS the diffusion is faster ($\eta _{\rm RD} \sim M_{\rm A}^{2}$). This work shows for the first time simulations of compressible MHD turbulence with the suppression of the cascade in the direction parallel to the mean magnetic field, which is consistent with incompressible weak turbulence theory. We also verified that in our simulations the energy cascading time does not follow the scaling with MA predicted for the weak regime, in contradiction with the RD theory assumption. Our results generally support and expand the RD theory predictions.

APA, Harvard, Vancouver, ISO, and other styles

42

Kiyani, Khurom H., Kareem T. Osman, and Sandra C. Chapman. "Dissipation and heating in solar wind turbulence: from the macro to the micro and back again." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 373, no. 2041 (May 13, 2015): 20140155. http://dx.doi.org/10.1098/rsta.2014.0155.

Full text

Abstract:

The past decade has seen a flurry of research activity focused on discerning the physics of kinetic scale turbulence in high-speed astrophysical plasma flows. By ‘kinetic’ we mean spatial scales on the order of or, in particular, smaller than the ion inertial length or the ion gyro-radius—the spatial scales at which the ion and electron bulk velocities decouple and considerable change can be seen in the ion distribution functions. The motivation behind most of these studies is to find the ultimate fate of the energy cascade of plasma turbulence, and thereby the channels by which the energy in the system is dissipated. This brief Introduction motivates the case for a themed issue on this topic and introduces the topic of turbulent dissipation and heating in the solar wind. The theme issue covers the full breadth of studies: from theory and models, massive simulations of these models and observational studies from the highly rich and vast amount of data collected from scores of heliospheric space missions since the dawn of the space age. A synopsis of the theme issue is provided, where a brief description of all the contributions is discussed and how they fit together to provide an over-arching picture on the highly topical subject of dissipation and heating in turbulent collisionless plasmas in general and in the solar wind in particular.

APA, Harvard, Vancouver, ISO, and other styles

43

Treumann, Rudolf A., Wolfgang Baumjohann, and Yasuhito Narita. "Inverse scattering problem in turbulent magnetic fluctuations." Annales Geophysicae 34, no. 8 (August 16, 2016): 673–89. http://dx.doi.org/10.5194/angeo-34-673-2016.

Full text

Abstract:

Abstract. We apply a particular form of the inverse scattering theory to turbulent magnetic fluctuations in a plasma. In the present note we develop the theory, formulate the magnetic fluctuation problem in terms of its electrodynamic turbulent response function, and reduce it to the solution of a special form of the famous Gelfand–Levitan–Marchenko equation of quantum mechanical scattering theory. The last of these applies to transmission and reflection in an active medium. The theory of turbulent magnetic fluctuations does not refer to such quantities. It requires a somewhat different formulation. We reduce the theory to the measurement of the low-frequency electromagnetic fluctuation spectrum, which is not the turbulent spectral energy density. The inverse theory in this form enables obtaining information about the turbulent response function of the medium. The dynamic causes of the electromagnetic fluctuations are implicit to it. Thus, it is of vital interest in low-frequency magnetic turbulence. The theory is developed until presentation of the equations in applicable form to observations of turbulent electromagnetic fluctuations as input from measurements. Solution of the final integral equation should be done by standard numerical methods based on iteration. We point to the possibility of treating power law fluctuation spectra as an example. Formulation of the problem to include observations of spectral power densities in turbulence is not attempted. This leads to severe mathematical problems and requires a reformulation of inverse scattering theory. One particular aspect of the present inverse theory of turbulent fluctuations is that its structure naturally leads to spatial information which is obtained from the temporal information that is inherent to the observation of time series. The Taylor assumption is not needed here. This is a consequence of Maxwell's equations, which couple space and time evolution. The inversion procedure takes advantage of a particular mapping from time to space domains. Though the theory is developed for homogeneous stationary non-flowing media, its extension to include flows, anisotropy, non-stationarity, and the presence of spectral lines, i.e. plasma eigenmodes like those present in the foreshock or the magnetosheath, is obvious.

APA, Harvard, Vancouver, ISO, and other styles

44

Bret, A., M. E. Dieckmann, and L. Gremillet. "Recent progresses in relativistic beam-plasma instability theory." Annales Geophysicae 28, no. 11 (November 24, 2010): 2127–32. http://dx.doi.org/10.5194/angeo-28-2127-2010.

Full text

Abstract:

Abstract. Beam-plasma instabilities are a key physical process in many astrophysical phenomena. Within the fireball model of Gamma ray bursts, they first mediate a relativistic collisionless shock before they produce upstream the turbulence needed for the Fermi acceleration process. While non-relativistic systems are usually governed by flow-aligned unstable modes, relativistic ones are likely to be dominated by normally or even obliquely propagating waves. After reviewing the basis of the theory, results related to the relativistic kinetic regime of the poorly-known oblique unstable modes will be presented. Relevant systems besides the well-known electron beam-plasma interaction are presented, and it is shown how the concept of modes hierarchy yields a criterion to assess the proton to electron mass ratio in Particle in cell simulations.

APA, Harvard, Vancouver, ISO, and other styles

45

Galeev, A. A. "Plasma Processes in the Outer Coma." International Astronomical Union Colloquium 116, no. 2 (1991): 1145–69. http://dx.doi.org/10.1017/s0252921100012860.

Full text

Abstract:

AbstractSpacecraft encounters with comets Giacobini-Zinner and Halley revealed a great variety of collective plasma phenomena accompanying the interaction of the solar wind with comets. In this review, we discuss the theory and in situ measurements of the Alfvén wave turbulence and the solar wind loading by cometary ions, and the structure of the cometary bow shock.

APA, Harvard, Vancouver, ISO, and other styles

46

XAPLANTERIS, CONSTANTINE L., and ELENI FILIPPAKI. "Nonlinear wavy phenomena into plasma: some cases of stabilization and control of chaotic behaviors." Journal of Plasma Physics 77, no. 5 (March 1, 2011): 679–92. http://dx.doi.org/10.1017/s0022377811000079.

Full text

Abstract:

AbstractStabilities, instabilities and turbulences have always appeared into a cylindrical magnetized argon plasma. These phenomena are caused by linear or nonlinear dynamics and are interpreted with the linear or nonlinear theory accordingly. In this paper, an experimental study accompanied by theoretical justification and based on the wave–wave interaction has been made; an azimuthally moved driving wave is enforced in a very simple way. The turbulence stabilization, the wave coupling, the instability synchronization and other wavy interactions, which are caused by using an external spatiotemporal electric signal, are presented. The research of the wavy subjects continuing in our laboratory aspires to comprehend the plasma chaotic behavior and take a step into suppressing the unstable inclination.

APA, Harvard, Vancouver, ISO, and other styles

47

Mikhailovskii, A. B., J. G. Lominadze, A. P. Churikov, V. D. Pustovitov, N. N. Erokhin, and S. V. Konovalov. "Kinetic theory of instabilities responsible for magnetic turbulence in laboratory rotating plasma." Physics Letters A 372, no. 21 (May 2008): 3846–51. http://dx.doi.org/10.1016/j.physleta.2008.02.052.

Full text

APA, Harvard, Vancouver, ISO, and other styles

48

Bakunin, Oleg G. "Quasilinear theory of plasma turbulence. Origins, ideas, and evolution of the method." Uspekhi Fizicheskih Nauk 188, no. 01 (March 2017): 55–87. http://dx.doi.org/10.3367/ufnr.2017.03.038096.

Full text

APA, Harvard, Vancouver, ISO, and other styles

49

Bakunin, O. G. "Quasilinear theory of plasma turbulence. Origins, ideas, and evolution of the method." Physics-Uspekhi 61, no. 1 (January 31, 2018): 52–83. http://dx.doi.org/10.3367/ufne.2017.03.038096.

Full text

APA, Harvard, Vancouver, ISO, and other styles

50

Mattor, Nathan, and Patrick H. Diamond. "Drift wave propagation as a source of plasma edge turbulence: Slab theory." Physics of Plasmas 1, no. 12 (December 1994): 4002–13. http://dx.doi.org/10.1063/1.870870.

Full text

APA, Harvard, Vancouver, ISO, and other styles

We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!