Computer Science
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.3565c&link_type=abstract
Spitzer Proposal ID #3565
Computer Science
Scientific paper
Massive stars inject energy into the ISM through UV radiation, fast stellar winds, and supernova blasts. This stellar energy feedback ionizes the ambient gas, sweeps it into shell structures, and fills the shell interior with hot, shock-heated gas. The interplay between massive star formation and stellar energy feedback plays an important role in the structure and evolution of the ISM in a galaxy. The Large Magellanic Cloud (LMC) provides an ideal site to study the stellar energy feedback process in star forming regions because individual massive stars can be resolved, classified, and inventoried and the associated interstellar structures can be studied both globally and in detail. We have been using the large sample of star forming regions in the LMC to carry out a multi-wavelength investigation of the structure of the ISM and the effects of stellar energy feedback. We find that the stellar energy input in superbubbles far exceeds the observed thermal and kinetic energies of the associated interstellar gas. We request IRAC and MIPS observations of a large sample of HII regions in the LMC in order to assess the stellar energy feedback at the earliest evolutionary stage and the role played by dust in the energy budget. These regions are selected to cover a wide range of evolutionary stages, structural complexity, and X-ray surface brightness. Specifically, we will (1) search for massive young stars and proto-stars, (2) examine how star formation proceeds spatially and temporally, (3) study the stellar energy feedback at the earliest evolutionary stages, (4) determine the distribution and temperature of dust in varied stellar UV radiation and interstellar X-ray radiation fields, and (5) assess the importance of dust on the thermal evolution of the ISM.
Chen Rosie Chang-Hui
Chu Y.-H. Y.-H.
Clayton Geoff
Dickel John
Dunne Bryan
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