Submillimetre emission and the dust content of compact H II regions

Details Submillimetre emission and the dust content of compact H II regions Submillimetre emission and the dust content of compact H II regions

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.251..584h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 251, Aug. 15, 1991, p. 584-599. Research supported by S

Astronomy and Astrophysics

Astronomy

27

Cosmic Dust, H Ii Regions, Infrared Sources (Astronomy), Massive Stars, Star Formation, Submillimeter Waves

Scientific paper

Submillimeter continuum observations of six compact H II regions are presented, most of which have been observed for the first time. These measurements fill the remaining gap between the IRAS observations and millimeter data and more fully define the energy distribution of the thermal dust emission in these objects. New models of compact H II regions are described in which photoionization models of the nebula are calculated self-consistently with the solution of the radiative transfer equation for the associated dust. These models are applied to the most well-studied object observed, G45.13 + 0.14 A. It is found that, assuming the exciting source is a single ZAMS star (Teff = 50,000 K), the model predicts far too high an excitation for the nebula as deduced from the IR fine-structure lines. A Teff of around 33,000 K is more appropriate, implying a cluster of stars, which in turn implies that the dust-to-gas ratio inside the ionized zone must be much lower that the canonical value of 0.007 estimated for the diffuse ISM. The models show that a graphite/silicate mixture cannot match the observed submillimeter emission whereas amorphous carbon/silicate can.

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