Volume 409, Number 2, October II 2003
|Page(s)||589 - 598|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
The physical structure of high-mass star-forming cores
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: firstname.lastname@example.org, email@example.com
Corresponding author: J. Hatchell, firstname.lastname@example.org
Accepted: 11 July 2003
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 photometry including ISO-LWS spectra, maps at 450 and 850 , 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 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 ), while the continuum spectrum sometimes deviates (by ). Reliable models thus require all three kinds of data.
Key words: stars: formation / ISM: dust, extinction / ISM: Hii regions / ISM: molecules / ISM: structure
© ESO, 2003
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.