Abstract
The effects of OB stars on the physical state of the interstellar medium have been investigated using a time-dependent numerical simulation which includes explicit two-dimensional hydrodynamics and implicit, coupled radiative transfer and thermodynamics. Using the observed birthrates, OB stars are placed randomly in space and time on an 180 pc square numerical grid where they ionize and push ambient gas for the duration of their main sequence lifetimes. Though they contribute a minuscule amount of ionization, the B stars are efficient excavators of ambient matter because their initial Stroemgren radii are much smaller than the distance that the shock front around the H II region can travel in the stellar lifetime.
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