| Issue |
A&A
Volume 406, Number 3, August II 2003
|
|
|---|---|---|
| Page(s) | 1061 - 1070 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361:20030730 | |
| Published online | 17 November 2003 | |
A simplified numerical model of coronal energy dissipation based on reduced MHD
1
Institut d'Astrophysique Spatiale, CNRS – Université Paris-Sud, Bât. 121, 91405 Orsay Cedex, France
2
Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, 50125 Firenze, Italy
3
Istituto Nazionale Fisica della Materia, Sezione A, Università di Pisa, 56100 Pisa, Italy
4
Dipartimento di Fisica, Università di Pisa, 56100 Pisa, Italy
Corresponding author: E. Buchlin, eric.buchlin@ias.fr
Received:
7
November
2002
Accepted:
6
May
2003
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 Alfvén 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.
Key words: magnetohydrodynamics (MHD) / Sun: corona / Sun: flares / turbulence
© ESO, 2003
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