| dc.contributor.author |
Krishan, V |
|
| dc.date.accessioned |
2008-07-29T04:52:05Z |
|
| dc.date.available |
2008-07-29T04:52:05Z |
|
| dc.date.issued |
1996-12 |
|
| dc.identifier.citation |
Journal of Plasma Physics, Vol. 56, pp. 427 - 440 |
en |
| dc.identifier.issn |
0022-3778 |
|
| dc.identifier.uri |
http://hdl.handle.net/2248/2929 |
|
| dc.description.abstract |
Montgomery and co-workers have developed a framework to describe the steady state of a turbulent magnetofluid, without the usual recourse to linearization. Thus the magnetic and velocity fields emerge in their fully nonlinear form as a consequence of the selective decays of the invariants of the system. Using this statistical theory of magnetohydrodynamic turbulence, the pressure, magnetic and flow fields of a solar coronal loop have been determined. The spatial and time profiles of the loop pressure are derived. A comparison with the observed properties of the loops is made, whenever possible. |
en |
| dc.format.extent |
3894 bytes |
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| dc.format.mimetype |
application/pdf |
|
| dc.language.iso |
en |
en |
| dc.publisher |
Cambridge University Press |
en |
| dc.subject |
Solar coronal loops: models |
en |
| dc.subject |
Solar coronal loops: magnetohydrodynamics |
en |
| dc.title |
Modelling of a solar coronal loop |
en |
| dc.type |
Article |
en |