MHD turbulence in Saturn's magnetosheath downstream of a quasi-parallel bow shock

The origin of the MHD turbulence downstream of a quasi-parallel shock is in vestigated using plasma and magnetic field data taken by Voyagers 1 and 2 d uring their outbound traversals of the Saturn's magnetosheath. The characte ristics of the waves observed in that region are compared with those of the waves present (1) downstream of a quasi-perpendicular shock and (2) in the foreshock. The last comparison supplies direct evidence that the upstream waves, filling the foreshock are the main source of the magnetosheath turbu lence, immediately downstream of a quasi-parallel shock.