It has long been argued that massive stars terminate further star formation by destroying their natal clouds. It has also been argued that young massive stars trigger further star formation by compression of the ambient ISM as the hot, over-pressured circumstellar bubble expands away from a young O star. Recent new data from Spitzer combined with high resolution radio continuum and molecular line images are revealing a surprisingly detailed view of the structure of stellar wind-blown mid-infrared (MIR) bubbles around young massive O and B stars. In this talk I will look at the observationally determined radial structure and morphologies of three selected MIR bubbles. In particular, I will derive the destruction radii of PAHs and the extent of the PDR regions, derive the ages of the bubbles, and identify the likely ionizing stars and the populations of YSOs associated with each bubble. Comparisons will be made between predictions of evolutionary models of wind-blown bubbles and observations. Evidence for triggered star formation will be discussed and used to place lower limits on the ages of two bubbles.