Structure of molecular clouds. VII - Energy balance in clouds with star formation (Type IIb)

Details Structure of molecular clouds. VII - Energy balance in clouds with star formation (Type IIb) Structure of molecular clouds. VII - Energy balance in clouds with star formation (Type IIb)

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...124..247s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 124, no. 2, Aug. 1983, p. 247-255. Research sponsored by the Deutsche Forschun

Astronomy and Astrophysics

Astrophysics

4

Astronomical Models, Cosmic Dust, Molecular Clouds, Radiative Transfer, Star Formation, Thermodynamic Equilibrium, Heating, Magnetohydrodynamic Turbulence, Protostars, Radiant Cooling

Scientific paper

An observationally derived dust model is used to supplement a gas component model in the present study of prominent star formation molecular cloud thermal equilibrium, and the gas and dust temperatures are found to be similar. After discussing dust and gas heating and cooling processes previously suggested in the literature, their efficiency is judged in light of their ability to explain the thermal structure of the present model. The gas is found to cool by radiation, and is probably heated by magnetic processes such as either ambipolar diffusion or MHD turbulence. While the dust cools by radiation, its heating source is uncertain, and may be protostellar only if the star formation extends over a large part of the cloud. It may otherwise be due to MHD turbulence, if the dust grains are larger in the cloud than in the normal interstellar medium.

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