Abstract
Cometary ultracompact H II regions have been modelled as the interaction of the hypersonic wind from a moving star with the molecular cloud which surrounds the star. We here show that a similar morphology can ensue even if the star is stationary with respect to the cloud material. We assume that the H II region is within a stellar wind bubble which is strongly mass loaded: the cometary shape results from a gradient in the distribution of mass loading sources. This model circumvents problems associated with the necessarily high spatial velocities of stars in the moving star models.
| Original language | English |
|---|---|
| Pages (from-to) | 661-666 |
| Number of pages | 6 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 280 |
| Issue number | 2 |
| Publication status | Published - 1996 |
| Externally published | Yes |
Keywords
- H II regions
- Hydrodynamics
- ISM: Structure
- Radio lines: ISM
- Stars: Mass-loss