Five posters in the group of solar physics have been presented at this meeting on “Highly Energetic Physical Processes and Mechanisms for Emissions from Astrophysical Plasmas”. Four of these posters were dealing with aspects of solar flares, the most energetic processes observed in the solar corona, while one poster dealt with active regions. Although the most energetic particles in solar flares (E < 108 eV) do not compete with the most energetic cosmic rays (E > 1018.5 eV) observed in the rest of the universe, similar particle-acceleration mechanisms (electric fields, stochastic acceleration, shocks) are investigated for both phenomena. On the other hand, some highly efficient acceleration mechanisms operating in astrophysical plasmas (e.g., E x B drift in rapidly rotating B-fields on pulsars) are definitely not applicable to solar flares. However, a common theme in both astrophysical and solar acceleration processes is the role of magnetic reconnection, which was also the subject in one or the other form in all of the five presented solar posters. The joint venture of astrophysical and solar participants of this workshop contributed therefore nicely to a cross-fertilization of these common physical themes in both disciplines.