Clumpy ultracompact H II regions – I. Fully supersonic wind-blown models | Zendy

J. E. Dyson | Zendy; R. J. R. Williams | Zendy; M. P. Redman | Zendy

AI Assistant Blog Pricing

Home ZAIA Blog

Open Access

Clumpy ultracompact H II regions – I. Fully supersonic wind-blown models

Author(s) -

J. E. Dyson,

R. J. R. Williams,

M. P. Redman

Publication year - 1995

Publication title -

monthly notices of the royal astronomical society

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.058

H-Index - 383

eISSN - 1365-8711

pISSN - 0035-8711

DOI - 10.1093/mnras/277.2.700

Subject(s) - physics , astrophysics , supersonic speed , molecular cloud , star formation , choked flow , neighbourhood (mathematics) , high mass , astronomy , o type star , stellar wind , stars , mechanics , mathematical analysis , mathematics

We propose that a significant fraction of the ultracompact HII regions foundin massive star-forming clouds are the result of the interaction of the windand ionizing radiation from a young massive star with the clumpy molecularcloud gas in its neighbourhood. Distributed mass loading in the flow allows thecompact nebulae to be long-lived. In this paper, we discuss a particularlysimple case, in which the flow in the HII region is everywhere supersonic. Theline profiles predicted for this model are highly characteristic, for the caseof uniform mass loading. We discuss briefly other observational diagnostics ofthese models.

The content you want is available to Zendy users.

Already have an account? Click here to sign in.

Having issues? You can contact us here

Accelerating Research