Dust Processing Near Sites of High-Mass Star Formation in the Large Magellanic Cloud

Details Dust Processing Near Sites of High-Mass Star Formation in the Large Magellanic Cloud Dust Processing Near Sites of High-Mass Star Formation in the Large Magellanic Cloud

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20916001h&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #160.01; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a study into the properties of the dust and complex molecules in and around selected Hii regions in the Large Magellanic Cloud. The analysis is based on the Spitzer program SAGE (Surveying the Agents of a Galaxy's Evolution). Because of the lower metallicity environment, dust shielding is reduced and the effects of the ultraviolet radiation carry further than in the Milky way. Because of this these Hii regions may well be better representatives of star forming regions in the more distant universe.
We present the mid-IR spectral energy distributions (SEDs) as a function of radial distance to the center of the clusters: LHA 120-N4, N11, N63 and N105. These regions span a wide range in luminosities. The observed variations in SED are interpreted in terms of the varying incident radiation-field and changing abundances of polycyclic aromatic hydrocarbons (PAHs), transiently heated very small grains (VSG) to submicron-sized grains in thermal equilibrium, i.e. in terms of the varying grain-size distribution.
This analysis allows us to quantify the dust destruction and/or processing-rate due to photoevaporation and the typical distance scale on which Hii regions impact their surroundings.

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