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

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

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21713204l&link_type=abstract

American Astronomical Society, AAS Meeting #217, #132.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Observations demonstrate that star formation is an inefficient and slow process. This result can be attributed to the injection of energy and momentum that prevents free-fall collapse of molecular clouds. The mechanism of this feedback is debated theoretically: possible sources of pressure include the classical warm HII gas, the hot gas generated by shock-heating from stellar winds and supernovae, direct radiation from stars, and the dust-processed radiation field trapped inside the HII shell. In this talk, I present observational measurements of the pressures associated with each component listed above in the giant HII region 30 Doradus in the Large Magellanic Cloud. For this analyses, we have used high resolution, multi-wavelength images (radio, infrared, optical, and X-ray) to map these pressures as a function of position. We find that radiation pressure dominates within 50 pc of the central star cluster, R136, while the HII gas pressure dominates at larger radii. By contrast, the dust-processed radiation pressure and hot gas pressure are generally weak and not dynamically important, although the hot gas pressure may have played a more significant role at early times. I discuss the implications of these results regarding confinement/leakage of the hot gas from the HII shell and the early dynamics of 30 Dor.

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