Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21533202a&link_type=abstract
American Astronomical Society, AAS Meeting #215, #332.02; Bulletin of the American Astronomical Society, Vol. 42, p.430
Astronomy and Astrophysics
Astronomy
Scientific paper
The aim of this work is to give guidance to distinguish the existent theoretical models proposed for Ultracompact (UC) and Hypercompact (HC) HII regions based on present and future observational evidence. In this dissertation we focus in two of these models.
For a thick shell model we obtain the spectral energy distribution (SED), the angular size as a function of frequency and the intensity profile at centimeter wavelengths for a spherical ionized region bounded by an inner and an outer radius with an electron density gradient. We use our model to reproduce the observed properties of the ionized regions G34.26+0.15 A and B, and found that the model agrees with the observations. The main observational feature of this model is an off center peak intensity profile, marginally resolved on some observed HC HII regions.
For the photoevaporated disk wind model we calculate the SED, the Radio Recombination Line (RRL) profiles and both continuum
and RRL maps at centimeter wavelengths. We compare our results with observations of MWC 349 A to show that the model is consistent with the available observations, reproducing the continuum and line emission as well as the morphology of the source. The main observational features of this model are the morphology of the source and the broad RRL profile, found on most of the UC / HC HII on the literature and naturally explained by the gas dynamics of the photoevaporated disk wind.
More observations with higher spacial and spectral resolution and higher sensitivity are needed to determine the frequency of occurrence of this features in UC / HC HII regions. We briefly discuss the opportunity that the eVLA and ALMA radio interferometers would provide to study this early stage of the formation of massive stars.
Avalos Martin
Lizano Susana
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