The current generation of &ggr;‐ray telescopes (SIGMA, GRO) provides a new opportunity for observing red‐shifted &ggr;‐ray lines from the atmospheres of accreting neutron stars. A successful observation would provide important information about how the accretion stream settles onto the neutron star and might allow limits to be placed on the nuclear equation of state. Thus, we have undertaken a theoretical re‐analysis of different &ggr;‐ray emission mechanisms. This paper describe our results on the 4.438 MeV &ggr;‐ray line emission from12C and16O and outlines the ongoing calculation of the 2.2 MeV D‐recombination line flux expected from the spallation of incident Helium. We show that a neutron star accreting material of solar abundances will produce a 4.438 MeV &ggr;‐ray line flux that is below the current observational limits.