G. Mann¹, H.-T. Classen¹, U. Motschmann², Dröge³, and H. Kunow³

1 Astrophysikalisches Institut Potsdam, D-14482 Potsdam, Germany

2 Technische University Braunschweig, D-38106 Braunschweig, Germany

3 University Kiel, D-24118 Kiel, Germany

In the solar corona shock waves are generated either by flares and/or by coronal mass ejections. A numerical hybrid simulation of a quasi-parallel shock wave has been performed with typical coronal circumstances, i.e. with an Alfven-Mach number M_A = 4 and a low plasma beta b = 0.2. The simulation shows that strong magnetic field fluctuations appear at the vicinity of the shock transition. These fluctuations can act as magnetic mirrors at which electrons can be reflected and accelerated. Multiple encounters of electrons with such fluctuations lead to a considerable acceleration of them up to high energies of about 1 MeV as seen by a kinematic study of the relativistic electron movement between such magnetic mirrors. These theoretically obtained results are compared with measurements of the COSTEP instrument aboard the SOHO satellite. Especially, the COSTEP instrument has measured enhanced electron fluxes up to 3 MeV produced by a coronal shock wave during the solar event on July 9, 1996.