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Aluminium-26 is a short-lived radionuclide with a half-life of 0.72Myr, whichis observed today in the Galaxy via gamma-ray spectroscopy and is inferred tohave been present in the early Solar System via analysis of meteorites. Massivestars are considered the main contributors of Al26. Although most massive starsare found in binary systems, the effect, however, of binary interactions on theAl26 yields have not been investigated since Braun & Langer (1995). Here we aimto fill this gap. We have used the MESA stellar evolution code to computemassive (10Msun<=M<=80Msun), non-rotating, single and binary stars of solarmetallicity (Z=0.014). We computed the wind yields for the single stars and forthe binary systems where mass transfer plays a major role. Depending on theinitial mass of the primary star and orbital period, the Al26 yield can eitherincrease or decrease in a binary system. For binary systems with primary massesup to ~35-40Msun, the yield can increase significantly, especially at the lowermass-end, while above ~45Msun the yield becomes similar to the single staryield or even decreases. Our preliminary results show that compared tosupernova explosions, the contribution of mass-loss in binary systems to thetotal Al26 abundance produced by a stellar population is minor. On the otherhand, if massive star mass-loss is the origin of Al26 in the early SolarSystem, our results will have significant implications for the identificationof the potential stellar, or stellar population, source.

Aluminium-26 from massive binary stars I: non-rotating models