Impact of massive stars on the surrounding medium

We model nearby OB associations and their interactions with the ISM.
We have developed a population synthesis code using modern stellar
models to calculate the output of mass and energy from the massive
stars, and hydrodynamical simulations to follow the spread of ejecta
into the ISM. We aim to use observational constraints to constrain
the physics of the simulations, especially the radio-active tracer
26Al, with an average lifetime of 1 Myr, that is emitted in the winds
and supernova explosions of massive stars. The nearby Orion region
is one of the best observed such regions, and the massive stars
there have formed the Eridanus superbubble. We aim to use this region
for comparing theory and observations.