3 edition of Broken symmetry in ideal magnetohydrodynamic turbulence found in the catalog.
Broken symmetry in ideal magnetohydrodynamic turbulence
by National Aeronautics and Space Administration, Langley Research Center, National Technical Information Service, distributor in Hampton, Va, [Springfield, Va
Written in English
|Statement||John V. Shebalin.|
|Series||ICASE report -- no. 93-49., NASA technical memorandum -- 109017., ICASE report -- no. 93-49., NASA technical memorandum -- 109017.|
|Contributions||Langley Research Center.|
|The Physical Object|
Magnetofluid turbulence, broken symmetry and the dynamo problem John V. Shebalin from George Mason University, USA will be speaking. The problem of understanding if and how a magnetohydrodynamic (MHD) dynamo process could produce the Earth’s magnetic field was first proposed by Larmor in Ideal, homogeneous, magnetohydrodynamic turbulence is represented by finite Fourier series whose coefficients form a canonical ensemble. Here, the relevant statistical theory is substantially extended. This includes finding eigenvalues and eigenvectors of the covariance matrix for each modal probability density. The eigenvectors allow for a special unitary transformation of phase space.
NASA Johnson Space Center, Mail Code KA, Houston, TX Abstract. It is known that symmetries inherent in the statistical theory of ideal (i.e., non- dissipative) magnetohydrodynamic(MHD) turbulence are broken dynamically to produce coherent structure. Previous numerical investigations are extended to study decaying MHD turbulence. solar wind turbulence in the slow solar wind at two di erent heliocentric distances, 5 and 29 jer . The proof of this invariance for ideal magnetohydrodynamic equations depends on the symmetry is broken in the ﬂow. Because the value of these inviscid (ideal ﬂow) invariants cannot.
Self-organisation and non-linear dynamics in driven magnetohydrodynamic turbulent flows. Early considerations of freely decaying MHD turbulence involve the processes of selective decay . MHD, having three ideal invariants, is known to decay for very long times into different attractors depending on the initial ratio of these invariants. This symmetry breaking modiﬁes the scaling laws of the energy spectra at the peak of dissipation rate away from the k−2 scaling and towards the classical k−5/3 and k−3/2 power laws. DOI: /PhysRevE PACS number(s): Jv,Tv,−d I. INTRODUCTION In magnetohydrodynamic (MHD) turbulence several phe-.
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Get this from a library. Broken symmetry in ideal magnetohydrodynamic turbulence. [John V Shebalin; Langley Research Center.]. Book description. This book presents an introduction to, and modern account of, magnetohydrodynamic (MHD) turbulence, an active field both in general turbulence theory and in various areas of astrophysics.
The book starts by introducing the MHD equations, certain useful approximations and the transition to by: 6.
A sound knowledge is needed to tackle these problems. This work gives the basic information on turbulence in nature, comtaining the needed equations, notions and numerical simulations.
The current state of our knowledge and future implications of MHD turbulence Cited by: 4. Broken symmetry in ideal magnetohydrodynamic turbulence / By John V. Shebalin and Langley Research : John V.
Shebalin and Langley Research Center. The broken symmetry manifests itself as a coherent structure, i.e., a non-zero time-averaged part of the turbulent magnetic field.
The coherent structure is observed, in one case, to contain about eighteen percent of the total energyAuthor: John V. Shebalin. In summary, broken ergodicity in MHD turbulence leads to energetic, large-scale, quasistationary magnetic fields (coherent structures) in numerical models of bounded, turbulent magnetofluids.
Thus, broken ergodicity provides a large-scale dynamo mechanism within computer models of homogeneous MHD turbulence. These results may help us to better understand the origin of global magnetic fields. Phase space symmetries inherent in the statistical theory of ideal magnetohydrodynamic (MHD) turbulence are known to be broken dynamically to produce large-scale coherent magnetic structure.
Here, results of a numerical study of decaying MHD turbulence are presented that show large-scale coherent structure also arises and persists in the presence of dissipation. It is known that symmetries inherent in the statistical theory of ideal (i.e., non‐dissipative) magnetohydrodynamic (MHD) turbulence are broken dynamically to produce coherent structure.
Previous numerical investigations are extended to study decaying MHD turbulence. describe ideal, three-dimensional, magnetohydrodynamic (MHD) turbulence with and without rotation, and with and without a mean magnetic ﬁeld. Results from seven long-time numerical simulations of ﬁve general cases on a gridarepresen-ted.
One notable result is the discovery of a new ideal. We revisit the issue of the spectral slope of magnetohydrodynamic (MHD) turbulence in the inertial range and argue that the numerics favour a Goldreich–Sridhar −5/3 slope rather than a −3/2 slope.
We also perform precision measurements of the anisotropy of MHD turbulence and determine the anisotropy constant C A = of Alfvénic.
Absolute equilibrium ensemble theory for ideal homogeneous magnetohydrodynamic (MHD) turbulence is fairly well developed . Theory and simulation indicate that ideal MHD turbulence is non-ergodic and contains coherent structure.
The question of applicability to real (i.e., dissipative) MHD turbulence is examined. Results from several very long time numerical simulations on a 64^3 grid are. The results confirm that ideal magnetohydrodynamic turbulence is non-ergodic if there is no external magnetic field present.
This is due essentially to a canonical symmetry being broken in an arbitrary dynamical representation. The broken symmetry manifests itself as a coherent structure, i.e., a non-zero time-averaged part of the turbulent. Download Citation | Symmetry, statistics and structure in MHD turbulence | It is known that symmetries inherent in the statistical theory of ideal (i.e., non‐dissipative) magnetohydrodynamic.
Ideal magnetohydrodynamic (MHD) turbulence contains an intrinsic statistical mechanism called ‘broken ergodicity’ for producing an energetic, large-scale, quasi-stationary coherent structure.
Since MHD turbulence occurs in the Earth’s liquid outer core, the implication is that the Earth’s dipole magnetic field may be due to MHD turbulence, per se. Experiments on magnetohydrodynamic (MHD) turbulence have been made to study fundamental properties of the turbulence under the action of a strong magnetic field.
Although there are many well-known applications of MHD turbulence in metallurgy and related subjects, the number of such experiments that have been applied to the core is relatively small. Incompressible, homogeneous magnetohydrodynamic (MHD) turbulence consists of fluctuating vorticity and magnetic fi elds, which are represented in terms of their Fourier coefficients.
Here, a set of fi ve Fourier spectral transform method numerical simulations of two-dimensional (2-D) MHD turbulence on a $^2$ grid is described. Each simulation is a numerically realized dynamical system. Fourier analysis of incompressible, homogeneous magnetohydrodynamic (MHD) turbulence produces a model dynamical system on which to perform numerical experiments.
Statistical methods are used to understand the results of ideal (i.e., nondissipative) MHD turbulence simulations, with the goal of finding those aspects that survive the introduction. This book is a modern introduction to the ideas and techniques of quantum field theory.
Broken symmetry in ideal magnetohydrodynamic turbulence The results confirm that ideal. Magnetohydrodynamic turbulence concerns the chaotic regimes of magnetofluid flow at high Reynolds number.
Magnetohydrodynamics (MHD) deals with what is a quasi-neutral fluid with very high fluid approximation implies that the focus is on macro length-and-time scales which are much larger than the collision length and collision time respectively.
Abstract. The most interesting and probably the least understood flow problem is the turbulent flow. The essential characteristic of turbulent flow is that the turbulent fluctuations are random in nature; hence, the final and logical solution of the turbulence problem requires.
Magnetohydrodynamic turbulence Dieter Biskamp After a brief outline of magnetohydrodynamic theory, this introductory book discusses the macroscopic aspects of MHD turbulence, and covers the small-scale scaling properties.Here, we focus on the tachocline, review the equilibrium statistical mechanics of ideal magnetohydrodynamic (MHD) turbulence , and use this to introduce a thermodynamics of MHD turbulence applicable to the solar ssible MHD, of course, must be used to understand the whole Sun, (e.g., ) used an anelastic spherical harmonics code that models the radiation and .The control of heated fluid is of interest in many fields of engineering, such as boiler and heat exchanger design.
The broken symmetry of a thermo-physical system within a multi-sized media could be used to control its physical characteristics. In the current study, the effects of magnetohydrodynamic (MHD) forces and nanoparticles on boiling in a subcooled region inside an upright annular.