scholarly journals Dynamo effect in decaying helical turbulence

2019 ◽  
Vol 4 (2) ◽  
Author(s):  
Axel Brandenburg ◽  
Tina Kahniashvili ◽  
Sayan Mandal ◽  
Alberto Roper Pol ◽  
Alexander G. Tevzadze ◽  
...  
Keyword(s):  
Helical Turbulence ◽  
Dynamo Effect

scholarly journals Compressible helical turbulence: Fastened-structure geometry and statistics

2021 ◽  
Vol 28 (3) ◽  
pp. 032302
Author(s):  
Jian-Zhou Zhu
Keyword(s):  
Helical Turbulence ◽  
Structure Geometry

scholarly journals Filaments and the Solar Dynamo

1998 ◽  
Vol 167 ◽  
pp. 406-414
Author(s):  
N. Seehafer
Keyword(s):  
Mean Field ◽  
Decisive Role ◽  
Dynamo Theory ◽  
Simultaneous Generation ◽  
Alpha Effect ◽  
Generation Region ◽  
The Mean ◽  
Numerical Bifurcation ◽  
Dynamo Effect

AbstractFilaments are a global phenomenon and their formation, structure and dynamics are determined by magnetic fields. So they are an important signature of the solar magnetism. The central mechanism in traditional mean-field dynamo theory is the alpha effect and it is a major result of this theory that the presence of kinetic or magnetic helicities is at least favourable for the effect. Recent studies of the magnetohydrodynamic equations by means of numerical bifurcation-analysis techniques have confirmed the decisive role of helicity for a dynamo effect. The alpha effect corresponds to the simultaneous generation of magnetic helicities in the mean field and in the fluctuations, the generation rates being equal in magnitude and opposite in sign. In the case of statistically stationary and homogeneous fluctuations, in particular, the alpha effect can increase the energy in the mean magnetic field only under the condition that also magnetic helicity is accumulated there. Generally, the two helicities generated by the alpha effect, that in the mean field and that in the fluctuations, have either to be dissipated in the generation region or to be transported out of this region. The latter may lead to the appearance of helicity in the atmosphere, in particular in filaments, and thus provide valuable information on dynamo processes inaccessible to in situ measurements.

On the problem of magnetic field generation by helical turbulence

1995 ◽  
Vol 81 (1-2) ◽  
pp. 101-112 ◽  
Author(s):  
M. V. Kurgansky
Keyword(s):  
Magnetic Field ◽  
Magnetic Field Generation ◽  
Field Generation ◽  
Helical Turbulence

Oscillatory mean-field dynamos with a spherically symmetric, isotropic helical turbulence parameterα

2003 ◽  
Vol 67 (2) ◽  
Author(s):  
Frank Stefani ◽  
Gunter Gerbeth
Keyword(s):  
Mean Field ◽  
Spherically Symmetric ◽  
Helical Turbulence

scholarly journals The Twists and Turns of the Dynamo Effect

Physics ◽  
2012 ◽  
Vol 5 ◽  
Author(s):  
Andreas Tilgner
Keyword(s):  
Dynamo Effect

scholarly journals Angular Momentum Transport and Dynamo Effect in Kepler Disks

2001 ◽  
Vol 200 ◽  
pp. 410-414
Author(s):  
Günther Rüdiger ◽  
Udo Ziegler
Keyword(s):  
Angular Momentum ◽  
Accretion Disks ◽  
Large Scale ◽  
Spherical Model ◽  
Momentum Transport ◽  
Rotational Instability ◽  
Jet Formation ◽  
Angular Momentum Transport ◽  
Dynamo Effect ◽  
Background Shear

Properties have been demonstrated of the magneto-rotational instability for two different applications, i.e. for a global spherical model and a box simulation with Keplerian background shear flow. In both nonlinear cases a dynamo operates with a negative (positive) α-effect in the northern (southern) disk hemisphere and in both cases the angular momentum transport is outwards. Keplerian accretion disks should therefore exhibit large-scale magnetic fields with a dipolar geometry of the poloidal components favoring jet formation.

scholarly journals Polarized Cosmological Gravitational Waves from Primordial Helical Turbulence

2005 ◽  
Vol 95 (15) ◽  
Author(s):  
Tina Kahniashvili ◽  
Grigol Gogoberidze ◽  
Bharat Ratra
Keyword(s):  
Gravitational Waves ◽  
Helical Turbulence

Lagrangian velocity covariance in helical turbulence

1977 ◽  
Vol 81 (2) ◽  
pp. 385-398 ◽  
Author(s):  
Robert H. Kraichnan
Keyword(s):  
Correlation Time ◽  
Perturbation Expansion ◽  
Direct Interaction ◽  
Helical Turbulence ◽  
Quantitative Accuracy ◽  
Lagrangian Velocity ◽  
Thin Spherical Shell ◽  
Direct Interaction Approximation ◽  
Interaction Approximation ◽  
Substantial Factor

The effect of helicity on the Lagrangian velocity covarianceUL(t) in isotropic, normally distributed turbulence is examined by computer simulation and by a renormalized perturbation expansion forUL(t). The first term of the latter represents Corrsin's (1959) conjecture (extrapolated to allt), which relatesUL(t) to the Eulerian covariance and the distributionG(x, t) of fluid-element displacement. Truncation of the expansion at the first term yields the direct-interaction approximation forG(x, t). The expansion suggests that with or without helicity Corrsin's conjecture is valid ast→ ∞ and that in either caseUL(t) behaves asymptotically like$t^{-(r+\frac{3}{2})}$if the spectrum of the Eulerian field varies likekr+2at small wavenumbers. Corrsin's conjecture breaks down at small and moderatetif there is strong helicity while remaining accurate at alltin the mirror-symmetric case. Computer simulations for a frozen Eulerian field with spectrum confined to a thin spherical shell inkspace indicate that strong helicity induces an increase in the Lagrangian correlation time by a factor of approximately three. Direct-interaction equations are constructed for the Lagrangian space-time covariance and the resulting prediction forUL(t) is compared with the simulations. The effect of helicity is well represented quantitatively by the direct-interaction equations for small and moderatetbut not for larget. These frozen-field results imply good quantitative accuracy at alltin time-varying turbulence whose Eulerian correlation time is of the order of the eddy-circulation time. In turbulence with weak helicity, the directinteraction equations imply that the Lagrangian correlation of vorticity with initial velocity is more persistent thanUL(t), by a substantial factor.

Non-Riemannian generalizations of the Born–Infeld model and the meaning of the cosmological term

2017 ◽  
Vol 14 (07) ◽  
pp. 1750108 ◽  
Author(s):  
Diego Julio Cirilo-Lombardo
Keyword(s):  
Type Equation ◽  
Field Equations ◽  
Dynamical Equations ◽  
Primordial Magnetic Fields ◽  
Suitable Form ◽  
Theory Of Gravitation ◽  
Affine Action ◽  
Dynamo Effect ◽  
The Einstein Formula

Theory of gravitation based on a non-Riemannian geometry with dynamical torsion field is geometrically analyzed. To this end, the simplest Lagrangian density is introduced as a measure (reminiscent of a sigma model) and the dynamical equations are derived. Our goal is to rewrite this generalized affine action in a suitable form similar to the standard Born–Infeld (BI) Lagrangian. As soon as the functional action is rewritten in the BI form, the dynamical equations lead the trace-free GR-type equation and the field equations for the torsion, respectively: both equations emerge from the model in a sharp contrast with other attempts where additional assumptions were heuristically introduced. In this theoretical context, the Einstein [Formula: see text], Newton [Formula: see text] and the analog to the absolute [Formula: see text]-field into the standard BI theory all arise from the same geometry through geometrical invariant quantities (as from the curvature [Formula: see text]). They can be clearly identified and correctly interpreted both physical and geometrically. Interesting theoretical and physical aspects of the proposed theory are given as clear examples that show the viability of this approach to explain several problems of actual interest. Some of them are the dynamo effect and geometrical origin of [Formula: see text] term, origin of primordial magnetic fields and the role of the torsion in the actual symmetry of the standard model. The relation with gauge theories, conserved currents, and other problems of astrophysical character is discussed with some detail.

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