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Observations show that star formation is an inefficient and slow process.This result can be attributed to the injection of energy and momentum by starsthat prevents free-fall collapse of molecular clouds. The mechanism of thisstellar feedback is debated theoretically: possible sources of pressure includethe classical warm HII gas, the hot gas generated by shock-heating from stellarwinds and supernovae, direct radiation of stars, and the dust-processedradiation field trapped inside the HII shell. In this paper, we measureobservationally the pressures associated with each component listed aboveacross the giant HII region 30 Doradus in the Large Magellanic Cloud. Weexploit high-resolution, multi-wavelengh images (radio, infrared, optical, andX-ray) to map these pressures as a function of position. We find that radiationpressure dominates within 75 pc of the central star cluster, R136, while theHII gas pressure dominates at larger radii. By contrast, the dust-processedradiation pressure and hot gas pressure are generally weak and not dynamicallyimportant, although the hot gas pressure may have played a more significantrole at early times. Based on the low X-ray gas pressures, we demonstrate thatthe hot gas is only partially confined and must be leaking out the HII shell.Additionally, we consider the implications of a dominant radiation pressure onthe early dynamics of 30 Doradus.

What Drives the Expansion of Giant HII Regions?: A Study of Stellar Feedback in 30 Doradus