We suggest a possible technique for remotely observing the acceleration of solar energetic ions toE>1&hthinsp;MeVat coronal shock fronts. It involves the observation of the wings of line emission from ions accelerated in shocks, which could be done with the UVCS experiment on the SOHO spacecraft. UVCS has two UV channels producing stigmatic spectra from 42 arc min slits that can observe the Ly&agr; and O VI lines, both of which could be broadened with the passage of a shock. In that case, the Ly&agr; line formation results from proton charge exchange and collisional excitation of hydrogen atoms, while the broadened O VI lines are due to directly acceleratedO5+ions. The search criterion for candidate SOHO events consists of UVCS observations of coronal regions flanking or ahead of fast(v>400&hthinsp;km/s)white light CMEs observed with the LASCO coronagraph. ©1999 American Institute of Physics.