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In solar energetic particle (SEP) events, the power-law dependence of elementabundance enhancements on their mass-to-charge ratios A/Q provides a new toolthat measures the combined rigidity dependences from both acceleration andtransport. Distinguishing these two processes can be more challenging. However,the effects of acceleration dominate when SEP events are small or when the ionseven propagate scatter-free, and transport can dominate the time evolution oflarge events with streaming-limited intensities. Magnetic reconnection in solarjets produces positive powers of A/Q from +2 to +7 and shock accelerationproduces mostly negative powers from -2 to +1 in small and moderate SEP eventswhere transport effects are minimal. This variation in the rigidity dependenceof shock acceleration may reflect the non-planer structure, complexity, andtime variation of coronal shocks themselves. Wave amplification by streamingprotons in the largest SEP events suppresses the escape of ions with low A/Q,creating observed powers of A/Q from +1 to +3 upstream of the acceleratingshock, decreasing to small negative powers downstream. Of course, the powers ofA/Q are correlated with the spectral indices of He, O, and Fe, yet unexplaineddepartures exist.

Distinguishing the Rigidity Dependences of Acceleration and Transport in Solar Energetic Particles