The physical structure of high-mass star-forming cores

Free access article

Issue		A&A Volume 409, Number 2, October II 2003


Page(s)		589 - 598
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20031106

A&A 409, 589-598 (2003)
DOI: 10.1051/0004-6361:20031106

The physical structure of high-mass star-forming cores

J. Hatchell and F. F. S. van der Tak

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: hatchell@mpifr-bonn.mpg.de, vdtak@mpifr-bonn.mpg.de
(Received 4 April 2003 / Accepted 11 July 2003)

Abstract
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 $\mu{\rm m}$ photometry including ISO-LWS spectra, maps at 450 and 850 $\mu{\rm m}$ , 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 $n(r)\propto r^{-p}$ 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 $\pm 0.25$ ), while the continuum spectrum sometimes deviates (by $\pm 0.5$ ). Reliable models thus require all three kinds of data.

Key words: stars: formation -- ISM: dust, extinction -- ISM: HII regions -- ISM: molecules -- ISM: structure

Offprint request: J. Hatchell, hatchell@mpifr-bonn.mpg.de

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