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dc.contributor.authorTsiklauri, Den_US
dc.date.accessioned2016-04-12T12:32:53Z
dc.date.issued2006-07-01en_US
dc.date.submitted2016-03-23T12:15:27.869Z
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/11783
dc.descriptionpresentation at SOHO17, Giardini Naxos, Sicily, 7-12 May, 2006, to appear in SOHO17 proceedings
dc.descriptionpresentation at SOHO17, Giardini Naxos, Sicily, 7-12 May, 2006, to appear in SOHO17 proceedingsen_US
dc.descriptionpresentation at SOHO17, Giardini Naxos, Sicily, 7-12 May, 2006, to appear in SOHO17 proceedingsen_US
dc.descriptionpresentation at SOHO17, Giardini Naxos, Sicily, 7-12 May, 2006, to appear in SOHO17 proceedingsen_US
dc.description.abstractUsing Particle-In-Cell simulations i.e. in the kinetic plasma description the discovery of a new mechanism of parallel electric field generation was recently reported. Here we show that the electric field generation parallel to the uniform unperturbed magnetic field can be obtained in a much simpler framework using the ideal magnetohydrodynamics (MHD) description. In ideal MHD the electric field parallel to the uniform unperturbed magnetic field appears due to fast magnetosonic waves which are generated by the interaction of weakly non-linear Alfv\'en waves with the transverse density inhomogeneity. In the context of the coronal heating problem a new {\it two stage mechanism} of plasma heating is presented by putting emphasis, first, on the generation of parallel electric fields within an {\it ideal MHD} description directly, rather than focusing on the enhanced dissipation mechanisms of the Alfv\'en waves and, second, dissipation of these parallel electric fields via {\it kinetic} effects. It is shown that for a single Alfv\'en wave harmonic with frequency $\nu = 7$ Hz, and longitudinal wavelength $\lambda_A = 0.63$ Mm for a putative Alfv\'en speed of 4328 km s$^{-1}$, the generated parallel electric field could account for 10% of the necessary coronal heating requirement. We conjecture that wide spectrum (10$^{-4}-10^3$ Hz) Alfv\'en waves, based on the observationally constrained spectrum, could provide the necessary coronal heating requirement. By comparing MHD versus kinetic results we also show that there is a clear indication of the {\it anomalous resistivity} which is 100s of times greater than the classical Braginskii value.en_US
dc.relation.ispartofSOHO-17. 10 Years of SOHO and Beyond, Proceedings of the conference held 7-12 May, 2006 at Giardini Naxos, Sicily, Italy. Edited by H. Lacoste and L. Ouwehand. ESA SP-617. European Space Agency, 2006. Published on CDROM, p.111.1en_US
dc.subjectastro-phen_US
dc.subjectastro-phen_US
dc.titleMHD versus kinetic effects in the solar coronal heating: a two stage mechanismen_US
dc.typeArticle
pubs.author-urlhttp://arxiv.org/abs/astro-ph/0606658v1en_US
pubs.notesNot knownen_US
pubs.publication-statusPublisheden_US


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