Journal
SPACE SCIENCE REVIEWS
Volume 159, Issue 1-4, Pages 357-420Publisher
SPRINGER
DOI: 10.1007/s11214-011-9803-y
Keywords
Sun: flares; Sun: X-rays; Sun: acceleration; Sun: energetic particles
Categories
Funding
- NASA [NNX10AT78G]
- UC Berkeley
- PPARC/STFC UK
- Royal Society
- European Commission through the SOLAIRE Network [MTRN-CT-2006-035484]
- International Space Science Institute (ISSI) in Bern, Switzerland
- Centre National d'Etudes Spatiales (CNES)
- INSU/CNRS
- Science Technology and Facility Council (STFC) [PP/E001246/1]
- University of St Andrews, UK
- NASA [123023, NNX10AT78G] Funding Source: Federal RePORTER
- Science and Technology Facilities Council [ST/I001808/1, ST/F003064/1] Funding Source: researchfish
- STFC [ST/I001808/1, ST/F003064/1] Funding Source: UKRI
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We review basic theoretical concepts in particle acceleration, with particular emphasis on processes likely to occur in regions of magnetic reconnection. Several new developments are discussed, including detailed studies of reconnection in three-dimensional magnetic field configurations (e. g., current sheets, collapsing traps, separatrix regions) and stochastic acceleration in a turbulent environment. Fluid, test-particle, and particle-in-cell approaches are used and results compared. While these studies show considerable promise in accounting for the various observational manifestations of solar flares, they are limited by a number of factors, mostly relating to available computational power. Not the least of these issues is the need to explicitly incorporate the electrodynamic feedback of the accelerated particles themselves on the environment in which they are accelerated. A brief prognosis for future advancement is offered.
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