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Date and Time of the Query: 2019-05-23 T17:04:03 PDT
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For refcode 2011ApJ...731...91L:
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2011ApJ...731...91L What Drives the Expansion of Giant H II Regions?: A Study of Stellar Feedback in 30 Doradus Lopez, Laura A.; Krumholz, Mark R.; Bolatto, Alberto D.; Prochaska, J. Xavier; Ramirez-Ruiz, Enrico Abstract. Observations show that star formation is an inefficient and slow process. This result can be attributed to the injection of energy and momentum by stars that prevents free-fall collapse of molecular clouds. The mechanism of this stellar feedback is debated theoretically; possible sources of pressure include the classical warm H II gas, the hot gas generated by shock heating from stellar winds and supernovae, direct radiation of stars, and the dust-processed radiation field trapped inside the H II shell. In this paper, we measure observationally the pressures associated with each component listed above across the giant H II region 30 Doradus in the Large Magellanic Cloud. We exploit high-resolution, multi-wavelength images (radio, infrared, optical, ultraviolet, and X-ray) to map these pressures as a function of position. We find that radiation pressure dominates within 75 pc of the central star cluster, R136, while the H II 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. Based on the low X-ray gas pressures, we demonstrate that the hot gas is only partially confined and must be leaking out the H II shell. Additionally, we consider the implications of a dominant radiation pressure on the early dynamics of 30 Doradus. Key words: galaxies: star clusters: general, H II regions, ISM: individual objects: 30 Doradus, ISM: kinematics and dynamics, stars: formation, stars: massive
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