Relevant bibliographies by topics / Plasma physics- Alfvenic turbulence

Academic literature on the topic 'Plasma physics- Alfvenic turbulence'

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Published: 6 September 2023

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Journal articles on the topic "Plasma physics- Alfvenic turbulence"

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Valdés-Galicia, J. F., and R. A. Caballero. "Study of the magnetic turbulence in a corotating interaction region in the interplanetary medium." Annales Geophysicae 17, no. 11 (November 30, 1999): 1361–68. http://dx.doi.org/10.1007/s00585-999-1361-1.

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Abstract. We study the geometry of magnetic fluctuations in a CIR observed by Pioneer 10 at 5 AU between days 292 and 295 in 1973. We apply the methodology proposed by Bieber et al. to make a comparison of the relative importance of two geometric arrays of vector propagation of the magnetic field fluctuations: slab and two-dimensional (2D). We found that inside the studied CIR this model is not applicable due to the restrictions imposed on it. Our results are consistent with Alfvenic fluctuations propagating close to the radial direction, confirming Mavromichalaki et al.'s findings. A mixture of isotropic and magnetoacoustic waves in the region before the front shock would be consistent with our results, and a mixture of slab/2D and magnetoacoustic waves in a region after the reverse shock. We base the latter conclusions on the theoretical analysis made by Kunstmann. We discuss the reasons why the composite model can not be applied in the CIR studied although the fluctuations inside it are two dimensional.Key words. Solar physics · astrophysics and astronomy (magnetic fields) · Space plasma physics (turbulence; waves and instabilities)
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SCHLICKEISER, R., and F. JENKO. "Cosmic ray transport in non-uniform magnetic fields: consequences of gradient and curvature drifts." Journal of Plasma Physics 76, no. 3-4 (January 8, 2010): 317–27. http://dx.doi.org/10.1017/s0022377809990444.

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AbstractLarge-scale spatial variations of the guide magnetic field of interplanetary and interstellar plasmas give rise to the mirror force −(p⊥2/2mγB)∇B). The parallel component of this mirror force causes adiabatic focusing of the cosmic ray guiding center whereas the perpendicular component of the mirror force gives rise to the gradient and curvature drifts of the cosmic ray guiding center. Adiabatic focusing and the gradient and curvature drift terms additionally enter the Fokker–Planck transport equation for the gyrotropic cosmic ray particle phase space density in partially turbulent non-uniform magnetic fields. For magnetohydrodynamic turbulence with dominating magnetic fluctuations, the diffusion approximation is justified, which results in a modification of the diffusion–convection transport equation for the isotropic part of the gyrotropic phase space density from the additional focusing and drift terms. For axisymmetric undamped slab Alfvenic turbulence we show that all perpendicular spatial diffusion coefficients are caused by the non-vanishing gradient and curvature drift terms. For a specific (symmetric in μ) choice of the pitch-angle Fokker–Planck coefficients we show that the ratio of the perpendicular to parallel spatial diffusion coefficients apart from a constant is determined by the spatial first derivatives of the non-constant cosmic ray Larmor radius in the non-uniform magnetic field.
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SCHLICKEISER, R. "FIRST-ORDER DISTRIBUTED FERMI ACCELERATION OF COSMIC RAY HADRONS IN NON-UNIFORM MAGNETIC FIELDS." Modern Physics Letters A 24, no. 19 (June 21, 2009): 1461–72. http://dx.doi.org/10.1142/s0217732309031338.

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Large-scale spatial variations of the guide magnetic field of interplanetary and interstellar plasmas give rise to the adiabatic focusing term in the Fokker–Planck transport equation of cosmic rays. As a consequence of the adiabatic focusing term, the diffusion approximation to cosmic ray transport in the weak focusing limit gives rise to first-order Fermi acceleration of energetic particles if the product HL of the cross helicity state of Alfvenic turbulence H and the focusing length L is negative. The basic physical mechanisms for this new acceleration process are clarified and the astrophysical conditions for efficient acceleration are investigated. It is shown that in the interstellar medium this mechanism preferentially accelerates cosmic ray hadrons over 10 orders of magnitude in momentum. Due to heavy Coulomb and ionization losses at low momenta, injection or preacceleration of particles above the threshold momentum pc≃0.17Z2/3 GeV /c is required.
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Lysak, Robert L., and Mary K. Hudson. "Effect of double layers on magnetosphere–ionosphere coupling." Laser and Particle Beams 5, no. 2 (May 1987): 351–66. http://dx.doi.org/10.1017/s0263034600002822.

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The earth's auroral zone contains dynamic processes occurring on scales from the length of an auroral zone field line (about 10RE) which characterizes Alfven wave propagation to the scale of microscopic processes which occur over a few Debye lengths (less than 1 km). These processes interact in a time-dependent fashion since the current carried by the Alfven waves can excite microscopic turbulence which can in turn provide dissipation of the Alfven wave energy. This review will first describe the dynamic aspects of auroral current structures with emphasis on consequences for models of microscopic turbulence. In the second part of the paper a number of models of microscopic turbulence will be introduced into a large scale model of Alfven wave propagation to determine the effect of various models on the overall structure of auroral currents. In particular, we will compare the effect of a double layer electric field which scales with the plasma temperature and Debye length with the effect of anomalous resistivity due to electrostatic ion cyclotron turbulence in which the electric field scales with the magnetic field strength. It is found that the double layer model is less diffusive than the resistive model leading to the possibility of narrow, intense current structures.
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Venkatakrishnan, P. "Observable Signals of Coronal Heating Processes." Highlights of Astronomy 10 (1995): 305–6. http://dx.doi.org/10.1017/s1539299600011291.

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AbstractThe solar corona is thought to be sustained by waves, currents, turbulence or by velocity filtration. For efficient wave heating of the corona, only the Alfven waves seem to survive the effects of steepening and shock dissipation in the chromosphere (Zirker, 1993, Solar Phys. 148,43) and these can be dissipated in the corona by mode conversion or phase mixing (Priest, 1991 in XIV Consultation on Solar Physics, Karpacz). Enhanced line width of 530.3 nm coronal line seen within closed structures (Singh et al., 1982, J. Astrophys. Astron. 3,248), association of enhanced line width of HeI 1083 nm line with enhanced equivalent width (Venkatakrishnan et al., 1992, Solar Phys. 138,107), and gradients seen in the MgX 60.9 and 62.5 nm coronal line width (Hassler, et al., 1990, Astrophys. J. 348, L77), are possibly some examples of the observed signals of wave heating. Current sheets, produced in a variety of ways (Priest and Forbes, 1989, Solar Phys. 43,177; Parker, 1979, Cosmical Magnetic Fields, Ox. Univ. Press), can dissipate and provide heat. The properties of current sheets can be inferred from fill factors, emission measures (Cargill, 1994, in J.L. Burch and J.H. Waite, Jr. (eds.) Solar System Plasma Physics: Resolution of Processes in Space and Time, AGU Monograph), hard xrays (Lin et al., 1984, Astrophys. J. 283,421), and radio bursts (Benz, 1986, Solar Phys. 104,99). The association of large scale currents with enhanced transition region (deLoach et al., 1984, Solar Phys. 91,235.) and regions of enhanced magnetic shear with brighter corona (Moore et al., 1994, Proc. Kofu Symp) are of some possible interest in this context. Self consistent calculations of the turbulent cascade of energy from the scales of photospheric motions down into dissipative scales (Heyvaerts and Priest, 1992, Astrophys. J. 390,297) predict the width of coronal lines as a function of the properties of the forcing flows. Velocity filtration caused by free streaming effects off a non maxwellian boundary distribution of particles may well result in a plasma having coronal properties (Scudder, 1992a, Astrophys. J. 398,299; 1992b, Astrophys.J.11 398,319). The observable signals are the variation of line shapes with altitude.
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Leonovich, A. S., and D. A. Kozlov. "Alfvenic and magnetosonic resonances in a nonisothermal plasma." Plasma Physics and Controlled Fusion 51, no. 8 (July 21, 2009): 085007. http://dx.doi.org/10.1088/0741-3335/51/8/085007.

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SHAIKH, DASTGEER. "Dynamics of Alfvén waves in partially ionized astrophysical plasmas." Journal of Plasma Physics 76, no. 3-4 (December 18, 2009): 305–15. http://dx.doi.org/10.1017/s0022377809990493.

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AbstractWe develop a two dimensional, self-consistent, compressible fluid model to study evolution of Alfvenic modes in partially ionized astrophysical and space plasmas. The partially ionized plasma consists mainly of electrons, ions and significant neutral atoms. The nonlinear interactions amongst these species take place predominantly through direct collision or charge exchange processes. Our model uniquely describe the interaction processes between two distinctly evolving fluids. In our model, the electrons and ions are described by a single-fluid compressible magnetohydrodynamic (MHD) model and are coupled self-consistently to the neutral fluid via compressible hydrodynamic equations. Both plasma and neutral fluids are treated with different energy equations that adequately enable us to monitor non-adiabatic and thermal energy exchange processes between these two distinct fluids. Based on our self-consistent model, we find that the propagation speed of Alfvenic modes in space and astrophysical plasma is slowed down because these waves are damped predominantly due to direct collisions with the neutral atoms. Consequently, energy transfer takes place between plasma and neutral fluids. We describe the mode coupling processes that lead to the energy transfer between the plasma and neutral and corresponding spectral features.
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Similon, P. L., and R. N. Sudan. "Plasma Turbulence." Annual Review of Fluid Mechanics 22, no. 1 (January 1990): 317–47. http://dx.doi.org/10.1146/annurev.fl.22.010190.001533.

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Melatos, A., F. A. Jenet, and P. A. Robinson. "Electromagnetic strong plasma turbulence." Physics of Plasmas 14, no. 2 (February 2007): 020703. http://dx.doi.org/10.1063/1.2472293.

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Li, J. H., and Z. W. Ma. "Roles of super-Alfvenic shear flows on Kelvin–Helmholtz and tearing instability in compressible plasma." Physica Scripta 86, no. 4 (October 1, 2012): 045503. http://dx.doi.org/10.1088/0031-8949/86/04/045503.

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Dissertations / Theses on the topic "Plasma physics- Alfvenic turbulence"

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Kumari, Anju. "Localized structures and alfvenic turbulence in magnetized plasmas." Thesis, IIT Delhi, 2016. http://localhost:8080/xmlui/handle/12345678/7094.

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Nielson, Kevin Derek. "Analysis and gyrokinetic simulation of MHD Alfvén wave interactions." Diss., University of Iowa, 2012. https://ir.uiowa.edu/etd/3504.

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The study of low-frequency turbulence in magnetized plasmas is a difficult problem due to both the enormous range of scales involved and the variety of physics encompassed over this range. Much of the progress that has been made in turbulence theory is based upon a result from incompressible magnetohydrodynamics (MHD), in which energy is only transferred from large scales to small via the collision of Alfv ́n waves propagating oppositely along the mean magnetic field. Improvements in laboratory devices and satellite measurements have demonstrated that, while theories based on this premise are useful over inertial ranges, describing turbulence at scales that approach particle gyroscales requires new theory. In this thesis, we examine the limits of incompressible MHD theory in describing collisions between pairs of Alfvén waves. This interaction represents the fundamental unit of plasma turbulence. To study this interaction, we develop an analytic theory describing the nonlinear evolution of interacting Alfv ́n waves and compare this theory to simulations performed using the gyrokinetic code AstroGK. Gyrokinetics captures a much richer set of physics than that described by incompressible MHD, and is well-suited to describing Alfvénic turbulence around the ion gyroscale. We demonstrate that AstroGK is well suited to the study of physical Alfvén waves by reproducing laboratory Alfvén dispersion data collected using the LAPD. Additionally, we have developed an initialization alogrithm for use with AstroGK that allows exact Alfvén eigenmodes to be initialized with user specified amplitudes and phases. We demonstrate that our analytic theory based upon incompressible MHD gives excellent agreement with gyrokinetic simulations for weakly turbulent collisions in the limit that k⊥ ρi << 1. In this limit, agreement is observed in the time evolution of nonlinear products, and in the strength of nonlinear interaction with respect to polarization and scale. We also examine the effect of wave amplitude upon the validity of our analytic solution, exploring the nature of strong turbulence. In the kinetic limit where k⊥ ρi ≥ 1 where incompressible MHD is no longer a valid description, we illustrate how the nonlinear evolution departs from our analytic expression. The analytic theory we develop provides a framework from which more sophisticated of weak and strong inertial-range turbulence theories may be developed. Characterization of the limits of this theory may provide guidance in the development of kinetic Alfvén wave turbulence.
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Leonardis, Ersilia. "Quantifying finite range plasma turbulence." Thesis, University of Warwick, 2013. http://wrap.warwick.ac.uk/57673/.

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Turbulence is a highly non-linear process ubiquitous in Nature. The nonlinearity is responsible for the coupling of many degrees of freedom leading to an unpredictable dynamical evolution of a turbulent system. Nevertheless, experimental observations strongly support the idea that turbulence at small scales achieves a statistically stationary state. This has motivated scientists to adopt a statistical approach for the study of turbulence. In both hydrodynamics (HD) and magnetohydrodynamics (MHD), fluctuations of bulk quantities that describe turbulent flows exhibit the property of statistical scale invariance, which is a form of self-similarity. For fully evolved turbulence in an infinite medium, one interesting consequence of this scale invariance is the power law dependence of the physical observables of the flow such that, for instance, the velocity field fluctuations along a given direction show power law power spectra and multiscaling for the various orders of the structure function within a certain range of scales, known as the inertial range. The characterization of such scaling is crucial in turbulence since it would fully quantify the process itself, distinguishing the latter from a wider class of scaling processes (e.g., stochastic self-similar processes). Experimentally, it has been observed that turbulent systems exhibit an extended self-similarity when either turbulence is not completely evolved or the system has finite size. As consequence of this, the moments of the structure function exhibit a generalized scaling, which points to a universal feature of finite range MHD turbulent ows and, more generally, of scale invariant processes that have finite cut-offs of the fields or parameters. However, the underling physics of this generalized similarity is still an open question. This thesis focuses on the quantification of statistical scaling in turbulent systems of finite size. We apply statistical analyses to the spatio-temporal fluctuations associated with line of sight intensity measurements of a solar quiescent prominence and data of the reconnecting fields in simulations of magnetic reconnection. We find that in both environments these fluctuations exhibit the hallmarks of finite range turbulence. In particular, an extended self-similarity is observed to hold the inertial range of turbulence, which is consistent with a generalized scaling for the structure function. Importantly, this generalized scaling is found to be multifractal in character as a signature of intermittency in the turbulence cascade. The generalized scaling recovered for finite range turbulence exhibits dependence on a function, the generalized function, which contains important information about the bounded turbulent flow such as some characteristics scale of the flow, the crossover from the small scale to the outer scale of turbulence and perhaps some characteristic features of the boundaries (future work). The quantification of the generalized scaling is performed thank to the application of statistical tools, some of which have been here introduced for the first time, which allow to identify the statistical properties of a wide class of scaling processes. Importantly, these techniques are powerful methodologies for testing fractal/multifractal scaling in self-similar and quasi self-similar systems, allowing us to distinguish turbulence from other processes that show statistical scaling.
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Klein, Kristopher Gregory. "The kinetic plasma physics of solar wind turbulence." Diss., University of Iowa, 2013. https://ir.uiowa.edu/etd/5000.

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As means of investigating the various mechanisms which contribute to the persistence of magnetized turbulence in the solar wind, this dissertation details the development of tools through which turbulence theories can be directly compared to in situ observations. This comparison is achieved though the construction of synthetic spacecraft time series from spectra of randomly phased linear eigenmodes. A broad overview of the current understanding of plasma turbulence through analytic theory, spacecraft observation, and numerical simulation is presented with particular emphasis on previous uses of linear eigenmode characteristics in the literature. An analytic treatment of relevant fluid and kinetic linear waves follows, providing motivation for the choice of three eigenmode characteristics for studying solar wind turbulence in this dissertation. The novel synthetic spacecraft time series method is next detailed and its use in describing magnetized turbulence justified. The three metrics are then individually employed as a means of comparing the turbulence models used to generate synthetic time series with in situ observations. These comparisons provide useful constraints on various proposed mechanisms for sustaining the turbulence cascade and heating the solar wind plasma.
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Saucier, Antoine. "Cascade processes and fully developed turbulence." Thesis, McGill University, 1991. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=74674.

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The energy cascade process in turbulent flows is studied. Kolmogorov inertial range theories are critically reviewed and the multifractal characterization is discussed. Multiplicative cascade models are compared to the energy dissipation field (EDF) measured in the atmosphere. Landau's objection to the 1941 Kolmogorov theory is extended to the predictions of statistical fluid mechanics. The hypothesis $ rm Delta v( lambda L) { buildrel{d} over=} lambda sp{1/3} Delta v(L)$ is rejected with a statistical test. The moments $ rm langle( log varepsilon(L)) sp{p} rangle,$ where $ varepsilon$(L) denotes the EDF averaged over a volume of size L, are shown to be gaussian. For the EDF: Convergence tests showed that the exponents $ tau$(q) were not reliable for q $<$ 0; the correlations obey $ rm langle( mu sb{x}( delta)) sp{p}( mu sb{x+ delta}( delta)) sp{q} rangle propto delta sp{ gamma(p,q)}$ but $ gamma$ does not always equal the value obtained with a multinomial measure; a privileged scale ration r $ approx$ 1/2 is suggested by the prefactor oscillations of the correlation function. The implications of these results for the modelling of the EDF are discussed.
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Dewhurst, Joseph Michael. "Statistical description and modelling of fusion plasma edge turbulence." Thesis, University of Warwick, 2010. http://wrap.warwick.ac.uk/3903/.

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In tokamaks, heat and particle fluxes reaching the wall are often bursty and intermittent and understanding this behaviour is vital for the design of future reactors. Plasma edge turbulence plays an important role, its quantitative characterisation and modelling under different operating regimes is therefore an important area of research. Ion saturation current (Isat) measurements made in the edge region of the Large Helical Device (LHD) and Mega-Amp Spherical Tokamak (MAST) are analysed. Absolute moment analysis is used to quantify properties on different temporal scales of the measured signals, which are bursty and intermittent. In all data sets, two regions of power-law scaling are found, with the temporal scale τ≈40μs separating the two regimes. A monotonic relationship between connection length and skewness of the probability density function is found for LHD. A new numerical code, ‘HAWK,’ which solves the Hasegawa-Wakatani (HW) equations is presented. The HAWK code is successfully tested and used to study the HW model and modifications. The curvature-Hasegawa-Wakatani (CHW) equations include a magnetic field strength inhomogeneity, C = −∂lnB/∂x. The zonal-Hasegawa- Wakatani (ZHW) equations allow the self-generation of zonal flows. The statistical properties of the turbulent fluctuations produced by the HW model and variations thereof are studied. In particular, the probability density function of E × B density flux Γn = −n∂φ/∂y, structure functions, the bispectrum and transfer functions are investigated. Test particle transport is studied. For the CHW model, the conservation of potential vorticity Π = ∇2φ − n + (κ − C)x accounts for much of the phenomenology. Simple analytical arguments yield a Fickian relation Γn = (κ − C)Dx between the radial density flux Γn and the radial tracer diffusivity Dx. For the ZHW model, a subtle interplay between trapping in small scale vortices and entrainment in larger scale zonal flows determines the rate, character and Larmor radius dependence of the test particle transport. When zonal flows are allowed non-Gaussian statistics are observed. Radial transport (across the zones) is subdiffusive and decreases with the Larmor radius. Poloidal transport (along the zones), however, is superdiffusive and increases with small values of the Larmor radius.
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Williams, Timothy Joe. "Statistically constrained decimation of a turbulence model." W&M ScholarWorks, 1988. https://scholarworks.wm.edu/etd/1539623778.

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The constrained decimation scheme (CDS) is applied to a turbulence model. The CDS is a statistical turbulence theory formulated in 1985 by Robert Kraichnan; it seeks to correctly describe the statistical behavior of a system using only a small sample of the actual dynamics. The full set of dynamical quantities is partitioned into groups, within each of which the statistical properties must be uniform. Each statistical symmetry group is then decimated down to a small sample set of explicit dynamics. The statistical effects of the implicit dynamics outside the sample set are modelled by stochastic forces.;These forces are not totally random; they must satisfy statistical constraints in the following way: Full-system statistical moments are calculated by interpolation among sample-set moments; the stochastic forces are adjusted by an iterative process until decimated-system moments match these calculated full-system moments. Formally, the entire infinite heirarchy of moments describing the system statistics should be constrained. In practice, a small number of low-order moment constraints are enforced; these moments are chosen on the basis of physical insights and known properties of the system.;The system studied in this work is the Betchov model--a large set of coupled, quadratically nonlinear ordinary differential equations with random coupling coefficients. This turbulence model was originally devised to study another statistical theory, the direct interaction approximation (DIA). By design of the Betchov system, the DIA solution for statistical autocorrelation is easy to obtain numerically. This permits comparison of CDS results with DIA results for Betchov systems too large to be solved in full.;The Betchov system is decimated and solved under two sets of statistical constraints. Under the first set, basic statistical properties of the full Betchov system are reproduced for modest decimation strengths (ratios of full-system size to decimated-system size); however, problems arise at stronger decimation. These problems are solved by the second set of constraints. The second constraint set is intimately related to the DIA; that relationship is shown, and results from the CDS under those constraints are shown to approach the DIA results as the decimation strength increases.
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Gullman-Strand, Johan. "Turbulence and scalar flux modelling applied to separated flows." Doctoral thesis, Stockholm : Department of Mechanics, Royal Institute of Technology, 2004. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-92.

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Liu, Li. "Hierarchical structures in fully developed turbulence." Diss., The University of Arizona, 1999. http://hdl.handle.net/10150/289027.

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Analysis of the probability density functions (PDFs) of the velocity increment dvℓ and of their deformation is used to reveal the statistical structure of the intermittent energy cascade dynamics of turbulence. By analyzing a series of turbulent data sets including that of an experiment of fully developed low temperature helium turbulent gas flow (Belin, Tabeling, & Willaime, Physica D 93, 52, 1996), of a three-dimensional isotropic Navier-Stokes simulation with a resolution of 2563 (Cao, Chen, & She, Phys. Rev. Lett. 76, 3711, 1996) and of a GOY shell model simulation (Leveque & She, Phys. Rev. E 55, 1997) of a very big sample size (up to 5 billions), the validity of the Hierarchical Structure model (She & Leveque, Phys. Rev. Lett. 72, 366, 1994) for the inertial-range is firmly demonstrated. Furthermore, it is shown that parameters in the Hierarchical Structure model can be reliably measured and used to characterize the cascade process. The physical interpretations of the parameters then allow to describe differential changes in different turbulent systems so as to address non-universal features of turbulent systems. It is proposed that the above study provides a framework for the study of non-homogeneous turbulence. A convergence study of moments and scaling exponents is also carried out with detailed analysis of effects of finite statistical sample size. A quantity Pmin is introduced to characterize the resolution of a PDF, and hence the sample size. The fact that any reported scaling exponent depends on the PDF resolution suggests that the validation (or rejection) of a model of turbulence needs to carry out a resolution dependence analysis on its scaling prediction.
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Highcock, Edmund. "The zero-turbulence manifold in fusion plasmas." Thesis, University of Oxford, 2012. http://ora.ox.ac.uk/objects/uuid:7ed1774d-88a5-4764-ba06-1de00c348d26.

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The transport of heat that results from turbulence is a major factor limiting the temperature gradient, and thus the performance, of fusion devices. We use nonlinear simulations to show that a toroidal equilibrium scale sheared flow can completely suppress the turbulence across a wide range of flow gradient and temperature gradient values. We demonstrate the existence of a bifurcation across this range whereby the plasma may transition from a low flow gradient and temperature gradient state to a higher flow gradient and temperature gradient state. We show further that the maximum temperature gradient that can be reached by such a transition is limited by the existence, at high flow gradient, of subcritical turbulence driven by the parallel velocity gradient (PVG). We use linear simulations and analytic calculations to examine the properties of the transiently growing modes which give rise to this subcritical turbulence, and conclude that there may be a critical value of the ratio of the PVG to the suppressing perpendicular gradient of the velocity (in a tokamak this ratio is equal to q/ε where q is the magnetic safety factor and ε the inverse aspect ra- tio) below which the PVG is unable to drive subcritical turbulence. In light of this, we use nonlinear simulations to calculate, as a function of three parameters (the perpendicular flow shear, q/ε and the temperature gradient), the surface within that parameter space which divides the regions where turbulence can and cannot be sustained: the zero- turbulence manifold. We are unable to conclude that there is in fact a critical value of q/ε below which PVG-driven turbulence is eliminated. Nevertheless, we demonstrate that at low values of q/ε, the maximum critical temperature gradient that can be reached without generating turbulence (and thus, we infer, the maximum temperature gradient that could be reached in the transport bifurcation) is dramatically increased. Thus, we anticipate that a fusion device for which, across a significant portion of the minor radius, the magnetic shear is low, the ratio q/ε is low and the toroidal flow shear is strong, will achieve high levels of energy confinement and thus high performance.
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Books on the topic "Plasma physics- Alfvenic turbulence"

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1952-, Itoh S. I., and Itoh K, eds. Modern plasma physics. New York: Cambridge University Press, 2010.

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service), SpringerLink (Online, ed. Plasma Turbulence in the Solar System. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012.

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1952-, Itoh S. I., and Itoh K, eds. Plasma and fluid turbulence: Theory and modelling. Bristol: Institute of Physics Pub., 2003.

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Turbulence in space plasmas. Berlin: Springer, 2009.

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Spring College on Plasma Physics (1993 Trieste, Italy). Wave-particle interaction and energization in plasmas: Proceedings of the 4th week of the Spring College on Plasma Physics : Trieste, Italy, June 7-11, 1993. Edited by Shukla P. K. Stockholm: Royal Swedish Academy of Sciences, 1994.

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International Workshop on Small Scale Turbulence and Anomalous Transport in Magnetized Plasmas (1986 Institut d'études scientifiques de Cargèse). Turbulence and anomalous transport in magnetized plasmas: Proceedings of the International Workshop on Small Scale Turbulence and Anomalous Transport in Magnetized Plasmas held July 6-12th, 1986 at Institut dʼétudes scientifiques de Cargèse, Corse du Sud, France. [Palaiseau, France: L'Ecole Polytechnique], 1987.

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R, Gazis Paul, Phillips John L, and United States. National Aeronautics and Space Administration., eds. Constraints on solar wind acceleration mechanisms from Ulysses plasma observations: The first polar pass. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Moiseev, S. S. Nonlinear instabilities in plasmas and hydrodynamics. Bristol: Institute of Physics, 2000.

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S, Hasan S., Gangadhara R. T, and Krishan V, eds. Turbulence, dynamos, accretion disks, pulsars and collective plasmas processes: First Kodai-Trieste Workshop on Plasma Astrophysics held at the Kodaikanal Observatory, Kodaikanal, India, August 27 - September 7, 2007. [Berlin]: Springer, 2009.

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Barghouty, A. F. Coupled particle transport and pattern formation in a nonlinear leaky-box model. Huntsville], Ala: National Aeronautics and Space Administration, Marshall Space Flight Center, 2009.

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Book chapters on the topic "Plasma physics- Alfvenic turbulence"

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Miyamoto, Kenro. "Plasma Transport by Turbulence." In Plasma Physics for Controlled Fusion, 285–325. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-49781-4_13.

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Narita, Yasuhito. "Turbulence Properties in Space Plasma." In SpringerBriefs in Physics, 67–86. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-25667-7_4.

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Kono, Mitsuo, and Miloš M. Škorić. "Multifractal Characterization of Plasma Edge Turbulence." In Nonlinear Physics of Plasmas, 481–507. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-14694-7_14.

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Csernai, László P. "Turbulence in Low Viscosity Quark-Gluon Plasma." In Nuclear Physics: Present and Future, 175–81. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10199-6_17.

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Hasegawa, Akira, and Kinioki Mima. "Hydromagnetic Turbulence Associated with Plasma Discontinuities." In Physics of Solar Planetary Environments: Proceedings of the International Symposium on Solar-Terrestrial Physics, June 7-18,1976 Boulder, Colorado, Volume I, 505–10. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/sp007p0505.

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Held, G. A., C. D. Jeffries, and E. E. Haller. "Turbulence in Electron-Hole Plasma in Ge." In Proceedings of the 17th International Conference on the Physics of Semiconductors, 1289–92. New York, NY: Springer New York, 1985. http://dx.doi.org/10.1007/978-1-4615-7682-2_292.

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Dylov, Dmitry V., and Jason W. Fleischer. "Photonic Plasma Instabilities and Soliton Turbulence in Spatially Incoherent Light." In Localized States in Physics: Solitons and Patterns, 17–39. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-16549-8_2.

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Held, G. A., and C. D. Jeffries. "Chaos and Turbulence in an Electron-Hole Plasma in Germanium." In Complex Systems — Operational Approaches in Neurobiology, Physics, and Computers, 321–31. Berlin, Heidelberg: Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/978-3-642-70795-7_24.

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Ichimaru, Setsuo. "Plasma Turbulence." In Statistical Plasma Physics, 323–58. CRC Press, 2018. http://dx.doi.org/10.1201/9780429497155-9.

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Ichimaru, S. "Plasma Turbulence." In Basic Principles of Plasma Physics, 265–94. CRC Press, 2018. http://dx.doi.org/10.1201/9780429502118-11.

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Conference papers on the topic "Plasma physics- Alfvenic turbulence"

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Souza de Assis, Altair. "Turbulence-Double-Layer Synergetic Auroral Electron Acceleration." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1594022.

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Chian, A. C. L. "Onset of Alfvén Turbulence via Boundary Crisis." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1594030.

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Fujisawa, Akiihide. "Turbulence in Toroidal Plasma." In Proceedings of the 12th Asia Pacific Physics Conference (APPC12). Journal of the Physical Society of Japan, 2014. http://dx.doi.org/10.7566/jpscp.1.015005.

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Watanabe, T. H. "Direct Kinetic Simulations of Ion Temperature Gradient Driven Turbulence." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1593966.

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Dendy, R. O., Bengt Eliasson, and Padma K. Shukla. "Information Theory and Plasma Turbulence." In NEW DEVELOPMENTS IN NONLINEAR PLASMA PHYSICS: Proceedings of the 2009 ICTP Summer College on Plasma Physics and International Symposium on Cutting Edge Plasma Physics. AIP, 2009. http://dx.doi.org/10.1063/1.3266803.

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Naulin, Volker. "Electromagnetic Transport Components and Sheared Flows in Plasma Edge Turbulence." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1594008.

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Tsintsadze, N. L. "Strong Langmuir turbulence." In International conference on plasma physics ICPP 1994. AIP, 1995. http://dx.doi.org/10.1063/1.49045.

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Naulin, V. "Dynamics of Transport Barriers and ELM-Like Behaviour in Electrostatic Turbulence." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1594016.

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Shaikh, Dastgeer, P. K. Shukla, Bengt Eliasson, and Padma K. Shukla. "Turbulence in Hall MHD Plasmas." In NEW FRONTIERS IN ADVANCED PLASMA PHYSICS. AIP, 2010. http://dx.doi.org/10.1063/1.3533183.

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Otsuka, F. "Cross Field Diffusion of Cosmic Rays: Dependence on 2-D Field Turbulence Models." In PLASMA PHYSICS: 11th International Congress on Plasma Physics: ICPP2002. AIP, 2003. http://dx.doi.org/10.1063/1.1594053.

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