Stars in the halo of M31 are enriched with heavy elements a factor of ten more than the Milky Way halo. Many M31 globular clusters show high metallicities and enhanced nitrogen abundance, as does the M31 nucleus and near-nuclear regions. The bulk of the nitrogen comes from mass-loss in intermediate-mass asymptotic giant branch stars, a fairly quiescent process incapable of driving enriched gas out of a galaxy. We weigh the relative merits of supernova-wind-driven turbulent mixing versus in-situ large-galactocentric-radius enrichment to explain the observations.