Energy fluxes in helical magnetohydrodynamics and dynamo action

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dc.creatorVerma, Mahendra K.
dc.date2001-07-30
dc.date2004-04-25
dc.date.accessioned2026-07-07T11:10:39Z
dc.date.available2026-07-07T11:10:39Z
dc.descriptionRenormalized viscosity, renormalized resistivity, and various energy fluxes are calculated for helical magnetohydrodynamics using perturbative field theory. The calculation is to first-order in perturbation. Kinetic and magnetic helicities do not affect the renormalized parameters, but they induce an inverse cascade of magnetic energy. The sources for the the large-scale magnetic field have been shown to be (1) energy flux from large-scale velocity field to large-scale magnetic field arising due to nonhelical interactions, and (2) inverse energy flux of magnetic energy caused by helical interactions. Based on our flux results, a premitive model for galactic dynamo has been constructed. Our calculations yields dynamo time-scale for a typical galaxy to be of the order of $10^8$ years. Our field-theoretic calculations also reveal that the flux of magnetic helicity is backward, consistent with the earlier observations based on absolute equilibrium theory.
dc.descriptionREVTEX4; A factor of 2 corrected in helicity
dc.identifierhttps://arxiv.org/abs/nlin/0107069
dc.identifierhttp://arxiv.org/abs/nlin/0107069
dc.identifierPramana61:707-724,2003
dc.identifierdoi:10.1007/BF02706120
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/190838
dc.subjectChaotic Dynamics
dc.subjectAstrophysics
dc.subjectCondensed Matter
dc.titleEnergy fluxes in helical magnetohydrodynamics and dynamo action
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