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 Coronal Heating, Weak MHD Turbulence, and Scaling Laws

2007 ◽  
Vol 657 (1) ◽  
pp. L47-L51 ◽  
Author(s):  
A. F. Rappazzo ◽  
M. Velli ◽  
G. Einaudi ◽  
R. B. Dahlburg
Keyword(s):  
Scaling Laws ◽  
Coronal Heating ◽  
Mhd Turbulence

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

scholarly journals MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS

2013 ◽  
Vol 764 (1) ◽  
pp. 23 ◽  
Author(s):  
Igor V. Sokolov ◽  
Bart van der Holst ◽  
Rona Oran ◽  
Cooper Downs ◽  
Ilia I. Roussev ◽  
...  
Keyword(s):  
Turbulence Models ◽  
Coronal Heating ◽  
Mhd Turbulence ◽  
Magnetohydrodynamic Waves

scholarly journals Observations and Models of Coronal Heating

2001 ◽  
Vol 203 ◽  
pp. 456-466
Author(s):  
F. Malara ◽  
M. Velli
Keyword(s):  
Energy Release ◽  
Power Law ◽  
Magnetic Energy ◽  
Detection Threshold ◽  
Solar Radius ◽  
Coronal Heating ◽  
Fast Wave ◽  
Mhd Turbulence ◽  
Small Energy ◽  
Power Law Distributions

Energy release in the solar Corona is characterized by a sequence of space and time localized events, whose intensity follows power-law distributions. In quiet Sun regions, small energy events, possibly under the detection threshold, dominate, thus supporting the “nanoflare” scenario of coronal heating. Two complementar models of heating are discussed, in connection with the above observational features. The first model is based on Alfvénic wavepackets dissipation in 3D force-free magnetic fields; the presence of regions of chaoticity of magnetic lines allows for a fast wave dissipation, within a fraction of a solar radius. The second model describes a MHD turbulence in low-β plasma, in which magnetic energy is continuously furnished by slow photospheric motions. Energy release events corresponds dissipation of current sheets, often associated with magnetic reconnection. The resulting distribution of dissipated power follows a power law, similar to observations.

Coronal heating by quasi-2D MHD turbulence driven by non-WKB wave reflection

1999 ◽  
Author(s):  
William H. Matthaeus ◽  
Gary P. Zank ◽  
Sean Oughton
Keyword(s):  
Wave Reflection ◽  
Coronal Heating ◽  
Mhd Turbulence

scholarly journals Relaxed States of MHD Turbulence: Minimum Dissipation or Minimum Energy?

1990 ◽  
Vol 142 ◽  
pp. 215-222
Author(s):  
David Montgomery
Keyword(s):  
Steady State ◽  
Magnetic Energy ◽  
Minimum Energy ◽  
Energy Dissipation Rate ◽  
Relaxation Processes ◽  
Mhd Turbulence ◽  
Solar Prominences ◽  
Taylor Hypothesis ◽  
Reversed Field ◽  
Selective Decay

Driven, dissipative MHD fluids often seem to undergo relaxation processes. After a turbulent formation phase, a geometrically simpler and less disordered configuration emerges. The best known example is the laboratory reversed-field pinch (RFP); similar field topologies have been proposed for solar prominences and astrophysical “flux ropes.” In a transient situation, the more rapid decay of kinetic and magnetic energy relative to magnetic helicity provides a mechanism for generating an MHD configuration with several similarities to observed RFP states. (This is the Taylor hypothesis, not unrelated to turbulent inverse magnetic cascades.) For the driven steady state, however, all quantities are supplied at the same time-averaged rate at which they are dissipated, by definition; nothing decays relative to anything else. Some other unifying principle, beyond “minimum energy” or “selective decay,” seems necessary to describe the results of driven, steady-state MHD computations. We have been attempting to adapt the principle of minimum energy dissipation rate to MHD. It is a 19th century principle that achieved some success in hydrodynamics and separately in dissipative electrodynamics.

scholarly journals Coronal Heating by D.C. Currents

1990 ◽  
Vol 142 ◽  
pp. 207-214
Author(s):  
J. Heyvaerts
Keyword(s):  
Coronal Heating ◽  
Mhd Turbulence ◽  
Dc Current

Present views on DC current coronal heating are presented. The relation to AC mechanisms, the importance of MHD turbulence in both processes, and the convergence of presently proposed ideas is outlined.

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