Selective decay and dynamic alignment in the MHD turbulence: The role of the rugged invariants

2016 ◽  
Author(s):  
Daniele Telloni ◽  
Silvia Perri ◽  
Vincenzo Carbone ◽  
Roberto Bruno
Keyword(s):  
Mhd Turbulence ◽  
Selective Decay ◽  
Dynamic Alignment

Anomalous scaling and the role of intermittency in solar wind MHD turbulence: new insights

2007 ◽  
Author(s):  
C. Salem ◽  
A. Mangeney ◽  
S. D. Bale ◽  
P. Veltri ◽  
R. Bruno
Keyword(s):  
Solar Wind ◽  
Anomalous Scaling ◽  
Mhd Turbulence

scholarly journals Turbulence and dynamo interlinks

2012 ◽  
Vol 8 (S294) ◽  
pp. 337-348
Author(s):  
E. M. de Gouveia Dal Pino ◽  
R. Santos-Lima ◽  
G. Kowal ◽  
D. Falceta-Gonçalves
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Small Scale ◽  
Low Density ◽  
Mhd Turbulence ◽  
Turbulent Dynamo ◽  
Dynamo Process

AbstractThe role of turbulence in astrophysical environments and its interplay with magnetic fields is still highly debated. In this lecture, we will discuss this issue in the framework of dynamo processes. We will first present a very brief summary of turbulent dynamo theories, then will focus on small scale turbulent dynamos and their particular relevance on the origin and maintenance of magnetic fields in the intra-cluster media (ICM) of galaxies. In these environments, the very low density of the flow requires a collisionless-MHD treatment. We will show the implications of this approach in the turbulent amplification of the magnetic fields in these environments. To finalize, we will also briefly address the connection between MHD turbulence and fast magnetic reconnection and its possible implications in the diffusion of magnetic flux in the dynamo process.

scholarly journals Weakly imbalanced strong turbulence

2010 ◽  
Vol 6 (S274) ◽  
pp. 72-75
Author(s):  
Andrey Beresnyak
Keyword(s):  
High Resolution ◽  
Mhd Turbulence ◽  
3D Simulations ◽  
Numerical Evidence ◽  
Strong Turbulence ◽  
Dynamic Alignment

AbstractThe theory of strong MHD turbulence with cross-helicity has been a subject of many recent studies. In this paper we focused our attention on low-imbalance limit and performed high-resolution 3D simulations. The results suggest that in this limit both w+=v+b and w−=v−b are cascaded strongly. The model for imbalance based on so-called “dynamic alignment” strongly contradicts numerical evidence.

Coronal heating by selective decay of MHD turbulence

Solar Physics ◽  
1988 ◽  
Vol 116 (1) ◽  
Author(s):  
D. G�mez ◽  
C.Ferro Font�n
Keyword(s):  
Coronal Heating ◽  
Mhd Turbulence ◽  
Selective Decay

scholarly journals Cross-field transport and pitch-angle anisotropy of solar energetic particles in MHD turbulence

2016 ◽  
Vol 2 ◽  
pp. 63-65 ◽  
Author(s):  
F. Fraschetti
Keyword(s):  
Pitch Angle ◽  
Turbulence Models ◽  
Energetic Particles ◽  
Solar Energetic Particles ◽  
Mhd Turbulence ◽  
First Order ◽  
Angle Dependence ◽  
Inhomogeneous Turbulence ◽  
Angle Scattering

Abstract. Recent modelling of solar energetic particles (SEPs) propagation through the heliospheric turbulence, also discussed in this workshop, has investigated the role of the pitch-angle scattering and the perpendicular transport in spreading particles in heliolongitude, as shown by multi-spacecraft measurements (STEREO A/B, ACE, SOHO, etc.) at 1 AU in various energy ranges. In some events the first-order pitch-angle anisotropy of the particles distribution is not-negligible. We calculate the average perpendicular displacement due to the gradient/curvature drift in an inhomogeneous turbulence accounting for pitch-angle dependence for two MHD turbulence models: (a) 3-D isotropic, (b) anisotropic as conjectured by Goldreich-Sridhar. We find in both cases that the drift scales as (1 − μ2)2 with the cosine of pitch-angle μ, in contrast with previous models for transport of SEPs. This result can impact the models of propagation of SEPs through the heliosphere.

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