Solar gamma‐ray lines are produced through collisions of pairs of positive ions whose center of mass energies are above the relevant thresholds for excitation of gamma‐ray emitting states. Because of the low density of the solar plasma, prompt gamma rays are emitted by recoiling ions before significant energy loss has occurred. Thus, the lines are expected to be Doppler broadened to widths of the order of a hundred keV. Gamma‐ray lines resulting from proton and alpha‐particle (4He ion) beams on carbon and oxygen targets in the laboratory exhibit complex profiles which change rapidly with the gamma‐ray observation angle. Our earlier work has been limited to modeling laboratory and solar flare gamma‐ray profiles produced by proton excitation, but laboratory profiles of the carbon 4.44‐MeV line and oxygen 6.13‐MeV line from alpha excitation have now been successfully modeled. Solar flare gamma‐ray line profiles of the carbon and oxygen lines from heavy ions in the ambient solar medium interacting with representative high‐energy proton and alpha particle populations will be presented.