Solar Radio Bursts and Energetic Particle Events

With this entry cartoonist Ed Cliver enters the rarefied world of Cartoonists with Multiple Entries in this archive. He has, at least acronymically, become a CME himself! Note that this cartoon deals with particle acceleration, both near the reconnection region (CSHKP) but also at the flank of the interplanetary shock (oddly decoupled here and shown as a type II burst). Is this consistent with the artist's previous entry? Still something missing here though! There should be a blast wave running away from the flare; we might need this to explain the metric type II burst and the Moreton wave and in any case the physics requires it. Also the cartoon does not show particles coming from the shock front, as this paper explains; instead the arrow points clearly to particle acceleration on closed field lines, whence they could surely never escape because those field lines are closed. Now there is the interesting addition of the "quasi-perpendicular" region of the shock.
This condition might favor particle acceration, so this further confuses the issue: is particle acceleration happening at the shock, at the Q-perp flank, or at the reconnection point? Or at several places?

      Note: the original cartoon has been replaced by an improved version, not that its fundamental errors have been corrected.