Hollow H II regions. I - Effects of stellar evolution and wind energy dissipation

Details Hollow H II regions. I - Effects of stellar evolution and wind energy dissipation Hollow H II regions. I - Effects of stellar evolution and wind energy dissipation

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...160....1d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 160, no. 1, May 1986, p. 1-17. Research supported by Vrije Universiteit Brusse

Astronomy and Astrophysics

Astrophysics

41

Energy Dissipation, H Ii Regions, Mass Distribution, Stellar Evolution, Stellar Winds, B Stars, Nebulae, O Stars, Stellar Mass Ejection, Stellar Models

Scientific paper

Extended H II regions often exhibit a hollow structure: these bright nebulae consist of thick (e.g., Rosette nebula, Carina nebula), or thin (e.g. NGC 6888) ionized shells with an inner cavity and surrounded by neutral material. The exciting stars belong to OB associations; they are massive (up to several 10 M_sun;), and characterized by strong stellar winds. However, current models, in particular the classical "hot interstellar bubble", fail to account for the structure of these nebulae. The observations in fact suggest that the shock at the edge of the wind cavity is not adiabatic, like in these models, but must on the contrary be strongly dissipative. To solve this problem, the authors present in this work models based on two new developments. They apply their model to a number of definite objects: hollow H II regions like the Carina and Rosette nebulae, as well as thin "W-nebulae" around WR stars. The results show a good agreement with a variety of widely differing and independent observational constraints.

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