A simplified numerical model of coronal energy dissipation based on reduced MHD
arXiv:astro-ph/0212444 · doi:10.1051/0004-6361:20030730
Abstract
A 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.
arXiv comment11 pages, 9 figures Accepted for publication in Astronomy & Astrophysics
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- Energetic characterisation and statistics of solar coronal brightenings
- Modeling a coronal loop heated by MHD-turbulence nanoflares
- A Self-Organized-Criticality model consistent with statistical properties of edge turbulence in a fusion plasma
- Influence of the definition of dissipative events on their statistics
- Principle of Minimum Energy in Magnetic Reconnection in a Self-Organized Critical Model for Solar Flares
- Profiles of heating in turbulent coronal magnetic loops
- Energy Balance in Avalanche Models for Solar Flares
- On the ultraviolet signatures of small scale heating in coronal loops