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28 March 2024
 
  » arxiv » astro-ph/0509554

 Article overview


Starburst Models For FIR/sub-mm/mm Line Emission. I. An Expanding Supershell Surrounding A Massive Star Cluster
Lihong Yao ; T.A. Bell ; S. Viti ; J.A. Yates ; E.R. Seaquist ;
Date 19 Sep 2005
Subject astro-ph
AffiliationToronto), T.A. Bell, S. Viti, J.A. Yates (UCL), E.R. Seaquist (Toronto
AbstractThe effect of a newly born star cluster inside a giant molecular cloud (GMC) is to produce a hot bubble and a thin, dense shell of interstellar gas and dust swept up by the H II expansion, strong stellar winds, and repeated supernova explosions. Lying at the inner side of the shell is the photodissociation region (PDR), the origin of much of the far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) radiation from the interstellar medium (ISM). We present a model for the expanding shell at different stages of its expansion which predict mm/sub-mm and far-IR emission line intensities from a series of key molecular and atomic constituents in the shell. The kinematic properties of the swept-up shell predicted by our model are in very good agreement with the measurements of the supershell detected in the nearby starburst galaxy M 82. We compare the modeling results with the ratio-ratio plots of the FIR/sub-mm/mm line emission in the central 1.0 kpc region to investigate the mechanism of star forming activity in M 82. Our model has yielded appropriate gas densities, temperatures, and structure scales compared to those measured in M 82, and the total H2 content is compatible with the observations. This implies that the neutral ISM of the central star-forming region is a product of fragments of the evolving shells.
Source arXiv, astro-ph/0509554
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