Hα filtergrams and GOES X-ray observations of four homologous flares of May 28, 1980 are analysed. The Hα data gave us information about the spatial structure of the flares. The X-ray data were used to determine the temperature of flare plasma and to investigate its time variations. We have found that the duration of the high plasma:temperature are approximalely equal for all the four analysed flares. The Hα-structure of these flares was complicated
nevertheless we have found only slight changes of the structure from flare to flare. These resulls suggest that a common reviving source of the energy release is responsible for all the four homologous flares. The individual flares are due to successive revivals of the energy source. The conditions of the energy flow along the magnetic field lines emerging from the energy source
determine which parts of the chromosphere are seen in the
Hα emission.