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Recent observations of high ionization rates of molecular hydrogen in diffuseinterstellar clouds point to a distinct low-energy cosmic-ray component.Supposing that this component is made of nuclei, two models for the origin ofsuch particles are explored and low-energy cosmic-ray spectra are calculatedwhich, added to the standard cosmic ray spectra, produce the observedionization rates. The clearest evidence of the presence of such low-energynuclei between a few MeV per nucleon and several hundred MeV per nucleon in theinterstellar medium would be a detection of nuclear \gamma-ray line emission inthe range E_ 0.1 - 10 MeV, which is strongly produced in their collisions withthe interstellar gas and dust. Using a recent \gamma-ray cross sectioncompilation for nuclear collisions, \gamma-ray line emission spectra arecalculated alongside with the high-energy \gamma-ray emission due to {\pi} 0decay, the latter providing normalization of the absolute fluxes by comparisonwith Fermi-LAT observations of the diffuse emission above E \gamma = 0.1 GeV.Our predicted fluxes of strong nuclear \gamma-ray lines from the inner Galaxyare well below the detection sensitivies of INTEGRAL, but a detection,especially of the 4.4-MeV line, seems possible with new-generation \gamma-raytelescopes based on available technology. We predict also strong \gamma-raycontinuum emission in the 1-8 MeV range, which in a large part of our modelspace for low-energy cosmic rays exceeds considerably estimated instrumentsensitivities of future telescopes.

Deexcitation nuclear gamma-ray line emission from low-energy cosmic rays in the inner Galaxy