Magnetic fields in limb solar flares on heights 2–14 Mm

INTERFEROMETRY OF SOLAR FLARES AT 3-mm WAVELENGTH

K e y w o r d s : Sim: flares Sun: particle emission Sun: radio radiation

Solar Magnetic Fields

Magnetic reconnection configurations and particle acceleration in solar flares

Numerical simulations of two types of flares indicate that magnetic reconnection can provide environments favorable for various particle acceleration mechanisms to work. This paper reviews recent test particle simulations of DC electric field mechanism, and discusses how the flare particles can escape into the interplanetary space under different magnetic configurations.

Numerical Study of Magnetic Reconnection Processes in Solar Flares

Preface W. F. Ames (1965) said " fluid mechanics is especially rich in nonlinearities ". In this sense, I might as well say " Magnetohydrodynamics (MHD) is much richer ". Such rich nonlinearities bring about not only infinite research interest, but also enormous difficulty in mathematically treating them. Numerical simulation provides a powerful approach to overcome the difficulty and to invest...

Quasi - separatrix layers in solar flares II . Observed magnetic configurations

Weshow that the location ofHα orOVflare brightenings is related to the properties of the field-line linkage of the underlying magnetic region. The coronal magnetic field is extrapolated from the observed photospheric field assuming a linear force-free field configuration in order to determine the regions of rapid change in field-line linkage, called “quasi-separatrix layers” or QSLs. They are o...