Physics
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc...24n&link_type=abstract
Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam
Physics
Scientific paper
We discuss the origin of variations of the far-infrared [C II] line to far-infrared continuum and CO 1-0 line ratios observed in our Galaxy and in the Large Magellanic Cloud (LMC). The intensity ratio of the [C II] line emission to far-infrared continuum is systematically lower within the central several hundred parsecs of our Galaxy than that in the general Galactic plane. We attribute this relatively weak [C II] line emission to soft UV radiation with fewer C-ionizing photons in the Galactic center region. The soft radiation field, together with the pervasively high molecular gas density, makes the molecular self-shielding more effective in the Galactic center. The self-shielding raises the temperature of molecular gas at the C+/C/CO transition zone. We also mapped whole LMC, and showed that the mean [C II]/CO (1-0) line intensity ratio in the LMC is systematically larger than that in our Galaxy by an order of magnitude. We attribute this large [C II]/CO ratio to the lower dust abundance (and to lower metallicity) in the LMC, which allows UV photons to penetrate deeper into each clump of molecular clouds and convert more CO molecules into C+ ions.
Doi Yasuo
Low Frank J.
Mochizuki Kenji
Nakagawa Takao
Nishimura Takahiro
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