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We developed a new population synthesis code for groups of massive stars,where we model the emission of different forms of energy and matter from thestars of the association. In particular, the ejection of the two radioactiveisotopes 26Al and 60Fe is followed, as well as the emission of hydrogenionizing photons, and the kinetic energy of the stellar winds and supernovaexplosions. We investigate various alternative astrophysical inputs and theresulting output sensitivities, especially effects due to the inclusion ofrotation in stellar models. As the aim of the code is the application torelatively small populations of massive stars, special care is taken to addresstheir statistical properties. Our code incorporates both analytical statisticalmethods applicable to small populations, as well as extensive Monte Carlosimulations. We find that the inclusion of rotation in the stellar models has alarge impact on the interactions between OB associations and their surroundinginterstellar medium. The emission of 26Al in the stellar winds is stronglyenhanced, compared to non-rotating models with the same mass-loss prescription.This compensates the recent reductions in the estimates of mass-loss rates ofmassive stars due to the effects of clumping. Despite the lower mass-lossrates, the power of the winds is actually enhanced for rotating stellar models.The supernova power (kinetic energy of their ejecta) is decreased due to longerlifetimes of rotating stars, and therefore the wind power dominates oversupernova power for the first 6 Myr after a burst of star-formation. Forpopulations typical of nearby star-forming regions, the statisticaluncertainties are large and clearly non-Gaussian.

Using population synthesis of massive stars to study the interstellar medium near OB associations