We argue that Na is a potentially significant source of galactic axions. For temperatures K — characteristic of carbon burning in the massive progenitors of supernovae and ONeMg white dwarfs — the 440 keV first excited state of Na is thermally populated, with its repeated decays pumping stellar energy into escaping axions. Odd-A nuclear abundances are typically very low in high-temperature stellar environments (or absent entirely due to burn-up). Na is an exception: of the isotope is synthesized during carbon burning then maintained at K for times ranging up to y. Using MESA simulations, a galactic model, and sampling over progenitor masses, locations, and evolutionary stages, we find a continuous flux at earth of /cms for . Some fraction of these axions convert to photons as they propagate through the galactic magnetic field, producing a distinctive 440 keV line ray detectable by all-sky detectors like the Compton Spectrometer and Imager (COSI). Assuming a 1G galactic magnetic field and a sufficiently light axion mass, we find that COSI will be able to probe GeV at after two years of surveying.