A simplified numerical model of coronal energy dissipation based on reduced MHD

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dc.creatorBuchlin, E.
dc.creatorAletti, V.
dc.creatorGaltier, S.
dc.creatorVelli, M.
dc.creatorEinaudi, G.
dc.creatorVial, J. -C.
dc.date2002-12-19
dc.date2003-03-27
dc.date.accessioned2026-07-07T02:06:57Z
dc.date.available2026-07-07T02:06:57Z
dc.descriptionA 3D model intermediate between cellular automata (CA) models and the reduced magnetohydrodynamic (RMHD) equations is presented to simulate solar impulsive events generated along a coronal magnetic loop. The model consists of a set of planes distributed along a magnetic loop between which the information propagates through Alfven waves. Statistical properties in terms of power-laws for energies and durations of dissipative events are obtained, and their agreement with X-ray and UV flares observations is discussed. The existence of observational biases is also discussed.
dc.description11 pages, 9 figures Accepted for publication in Astronomy & Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/0212444
dc.identifierhttp://arxiv.org/abs/astro-ph/0212444
dc.identifierAstron.Astrophys. 406 (2003) 1061-1070
dc.identifierdoi:10.1051/0004-6361:20030730
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5539
dc.subjectAstrophysics
dc.titleA simplified numerical model of coronal energy dissipation based on reduced MHD
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