On the origin of time delays in hard X-ray and gamma-ray emission of solar flares

The possibility of a strong pitch-angle diffusion regime as well as of turbulent propagation of energetic ions and electrons in flaring loops has been shown. The strong diffusion regime suggests that two regions with a high level of small-scale turbulence are formed in the magnetic trap. Such additional 'turbulent mirrors' scatter energetic particles and, therefore, the flux of precipitating particles decreases and the mean lifetime of electrons and protons in a flaring loop grows. The possibility that the turbulent propagation of the particles can be responsible for the energy dependence of hard X-ray delays as well as the time lag of the gamma-ray line peaks with respect to the hard X-ray peaks as the electrons and ions are accelerated simultaneously cannot be ruled out. The trap plus the turbulent propagation model may also explain the lack of an abundant population of 10-100 keV electrons in interplanetary space in proton-rich events, and offers new possibilities for flare plasma diagnostics.