THE SPATIAL-DISTRIBUTION OF PARTICLES ACCELERATED BY CORONAL MASS EJECTION-DRIVEN SHOCKS

We use multispacecraft observations to examine the spatial and tempora l distributions of energetic particles accelerated by shock waves driv en by coronal mass ejections from the Sun. The behavior of the intensi ty time profiles ahead of the shock can depend strongly on the longitu de of the point where the observer's magnetic flux tube connects to th e shock, relative to the nose of the shock where acceleration is stron gest. Particle intensities can increase (decrease) with time as this p oint swings eastward through greater than or equal to 50 degrees towar d (away from) the shock nose because of solar rotation. Well behind th e shock, intensities are often constant with longitude and the intensi ties of these quasi-trapped particles at all energies decrease continu ously with time over many days as their containment volume expands. De layed proton events are produced when shocks expand into dow solar win d so they suddenly encounter an observer's field line far from the Sun . Sunward flows are seen when the shock passes over the observer or wh en it suddenly strikes his field line at radial distances out beyond h im.