Flare energy transport by conduction and radiation

Abstract

As energy is released in coronal flare loops, strong temperature gradients may appear and large-scale flows can be set up. In the absence of, or in addition to, energetic particle beams, thermal conduction and mass motions are major processes that distribute energy throughout the flare atmosphere. We review basic physical concepts of the energy transport processes, and their observational evidence. We then turn to radiative energy transport, an often ignored processes that may constitute a major transfer mechanism, particularly into and throughout the dense, optically thick, chromospheric and photospheric layers. The basic physics of radiative energy transport is reviewed, and some specific examples discussed in detail, particularly in connection with upper photosphere heating and white light flare events.