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Massive stars can alter physical conditions and properties of their ambientinterstellar dust grains via radiative heating and shocks. The HII regions inthe Large Magellanic Cloud (LMC) offer ideal sites to study the stellar energyfeedback effects on dust because stars can be resolved, and the galaxy's nearlyface-on orientation allows us to unambiguously associate HII regions with theirionizing massive stars. The Spitzer Space Telescope survey of the LMC providesmulti-wavelength (3.6 to 160 $\mu$m) photometric data of all HII regions. Toinvestigate the evolution of dust properties around massive stars, we haveanalyzed spatially-resolved IR dust emission from two classical HII regions(N63 and N180) and two simple superbubbles (N70 and N144) in the LMC. Weproduce photometric spectral energy distributions (SEDs) of numerous smallsubregions for each region based on its stellar distributions and nebularmorphologies. We use DustEM dust emission model fits to characterize the dustproperties. Color-color diagrams and model fits are compared with the radiationfield (estimated from photometric and spectroscopic surveys). Strong radialvariations of SEDs can be seen throughout the regions, reflecting the availableradiative heating. Emission from very small grains drastically increases atlocations where the radiation field is the highest, while polycyclic aromatichydrocarbons (PAHs) appear to be destroyed. PAH emission is the strongest inthe presence of molecular clouds, provided that the radiation field is low.

Spitzer Observations of Dust Emission from HII Regions in the Large Magellanic Cloud