Volume 467, Number 2, May IV 2007
|Page(s)||603 - 610|
|Section||Interstellar and circumstellar matter|
|Published online||02 November 2006|
Hα line profiles for a sample of supergiant HII regions
III. Model line profiles
Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, CP 22800, Baja California, Mexico e-mail: [maite;richer;wsteffen;ggs;jal]@astrosen.unam.mx
Accepted: 15 June 2006
We carried out a series of 1D hydrodynamical computations with the ZEUS fluid solver in order to reproduce the salient features in our high-resolution Hα emission line profiles of a sample of HII regions (see Rozas et al. 2006a,b). Four models were computed. In the first and second cases, an ionization-bounded HII region was modeled with and without a shell produced by stellar winds. In the third and fourth cases, a density-bounded HII region was considered, both with and without a shell driven by stellar winds. The resulting line profiles have been modeled using the SHAPE rendering program. We find that our observed high-quality profiles are well-reproduced in the density-bounded model that includes an expanding shell formed as a result of the stellar winds from the ionizing stars. Finally, we consider the effects that the finite slit widths used for the observations have on the physical conditions deduced from the line profile of the ionized bubble.
Key words: ISM: HII regions / ISM: kinematics and dynamics / stars: winds, outflows
© ESO, 2007
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.