Our Present Understanding of Solar Flares

Abstract

A general discussion of solar flares with emphasis on two-ribbon flares is given. The basic differences between compact (simple-loop) and two-ribbon flares have also been pointed. Skylab observations have been presented to show that the hot loops are seen first in X-rays, later in extreme ultraviolet lines and, after an appropriate cooling time, in H-aplha as the loop prominence systems. Particle acceleration during a long-enduring reconnection process in two-ribbon flares have been discussed.