Volume 471, Number 3, September I 2007
|Page(s)||993 - 997|
|Published online||26 June 2007|
Particle acceleration in solar flares: linking magnetic energy release with the acceleration process
LUTh, Observatoire de Paris, 92195 Meudon Cedex, France e-mail: email@example.com
Accepted: 21 May 2007
Context.Particles accelerated in solar flares draw their energy from the magnetic field. The dissipative scale of the magnetic energy in the solar corona implies that the magnetic energy is transmitted to the particles through a large number of dissipative regions (DR).
Aims.To finally compute the particle energy distribution, we present an approach to linking the magnetic energy release to the acceleration process that occurs in each DR .
Methods.Although not directly observed, the magnetic energy release process is assumed to evolve in an SOC state that leads to the power-law behaviour of the probability distribution function for the energy released in each DR. We consider that most of the accelerated particles leave the acceleration region after one interaction, but we introduce a distribution of the particle acceleration lengths inside each acceleration region.
Results.We calculate the kinetic energy distribution of the accelerated particles. Our model allows us to identify the physical process that determines each part of the particle energy distribution.
Conclusions.As a conclusion, we discuss the limitations of the approach presented in this paper.
Key words: Sun: flares / acceleration of particles
© ESO, 2007
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.