Abstract
By taking as a working hypothesis the existence of a fast process around a solar flare site, together with a longitudinal transport of low energy particles which is independent of particle energy and nearly independent of particle rigidity, a model is developed which is able to give a quantitative explanation of one group of observational features of the corona and a qualitative description of a second group. The former group of phenomena includes the increase of event onset time and maximum intensity with angular separation between observer and flare location, and the tendency of the azimuthal distribution of flare particles toward uniformity for large times during the decay phase of events. The latter group involves the spectral index of the power law energy spectra and the photospheric magnetic field sector control of the propagation of solar flare particles.
