The physical structure of high-mass star-forming cores

Details The physical structure of high-mass star-forming cores The physical structure of high-mass star-forming cores

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...409..589h&link_type=abstract

Astronomy and Astrophysics, v.409, p.589-598 (2003)

Astronomy and Astrophysics

Astrophysics

30

Stars: Formation, Ism: Dust, Extinction, Ism: Hii Regions, Ism: Molecules, Ism: Structure

Scientific paper

We present models of the temperature and density structure of the envelopes of ten deeply embedded massive stars associated with ultracompact HII regions. Constraints come from 60-1300 mum photometry including ISO-LWS spectra, maps at 450 and 850 mum , and CS emission line data. Radial profiles extracted from the maps after removing neighbouring sources were modelled taking the chopping process into account. The line data are modelled with a Monte Carlo program and the continuum data with a dust radiative transfer code. For an assumed n(r)~ r-p density structure, the index p is found to be uniformly distributed between 1.25 and 2.25 for this sample. The density power law index from radial profiles and emission lines agree well (by +/- 0.25), while the continuum spectrum sometimes deviates (by +/- 0.5). Reliable models thus require all three kinds of data.

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