Development of strongly dissipative MHD structures

The formation of compact magnetic structures by advection of an initial magnetic seed due to the motion of the plasma, and the intensification of the field due to line stretching are discussed. It is shown that when the plasma is squeezed locally by external agents, so that an inflow-outflow near a...

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Published inIEEE transactions on plasma science Vol. 20; no. 6; pp. 882 - 890
Main Authors Gratton, F.T., Gnavi, G., Bender, L.
Format Journal Article
LanguageEnglish
Published New York, NY IEEE 01.12.1992
Institute of Electrical and Electronics Engineers
Subjects
Astronomy
Conductivity
Earth, ocean, space
Exact sciences and technology
Fundamental aspects of astrophysics
Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations
Heat transfer
Hydrodynamics
Magnetic fields
Magnetic flux
Magnetic switching
Magnetohydrodynamics
Magnetohydrodynamics and plasmas
Nuclear and plasma sciences
Numerical analysis
Q1
Slabs
Steady-state
Plasma
Current sheet
Plasma flow
Solar atmosphere
Stagnation point flow
Solar prominence
Similarity solution
Energy transfer
Selfsimilarity
Magnetic energy
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Summary:The formation of compact magnetic structures by advection of an initial magnetic seed due to the motion of the plasma, and the intensification of the field due to line stretching are discussed. It is shown that when the plasma is squeezed locally by external agents, so that an inflow-outflow near a stagnation point is generated by the pinching, large amounts of Joule heating are obtained in a short time when the magnetic Reynolds number is large.< >
Bibliography:ObjectType-Article-2
SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 23
ISSN:0093-3813
1939-9375
DOI:10.1109/27.199543