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http://hdl.handle.net/2248/2929
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DC Field | Value | Language |
---|---|---|
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 | - |
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 |
Appears in Collections: | IIAP Publications |
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