Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-23T18:58:50.873Z Has data issue: false hasContentIssue false
  • English
  • Français

Hollow H II Regions: From Giant to Ultracompact

Published online by Cambridge University Press:  04 August 2017

T. Montmerle ,
H. Dorland  and
C. Doom
T. Montmerle
Affiliation:
Centre d'Etudes Nucléaires de Saclay, France
H. Dorland
Affiliation:
Centre d'Etudes Nucléaires de Saclay, France
C. Doom
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Belgium

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

H II regions around OB associations have a thick-shell structure (see, e.g., the Carina and Rosette nebulae), and yet the standard “Hot Interstellar Bubble” model (e.g., Weaver et al. 1977) predicts thin H II shells around a large X-ray emitting volume, when associated with stellar winds. Observations suggest that strong dissipation must occur at the edge of the wind cavity: (i) expansion velocities there are much smaller than predicted by the standard model (e.g., Chu, 1983); (ii) in bubbles around WR stars, overabundances of N, He, etc., are seen, hence the need to cool these WR-produced elements down to observable temperatures (Kwitter, 1981). Also, two theoretical developments are important: (i) new stellar evolution models for massive stars, including mass loss and overshooting in convective cores (e.g., Doom, 1985); (ii) a non-linear theory for heat conduction with steep temperature gradients (Luciani et al. 1985).

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 198 - 200
Copyright
Copyright © Reidel 1987 

References

Celnik, W.E.: 1985, Astron. Astrophys. 144, 171.Google Scholar
Chu, Y.M.: 1983, Astrophys. J. 269, 202.CrossRefGoogle Scholar
Doom, C.: 1985, Astron. Astrophys. 142, 143.Google Scholar
Doom, C. et al.: 1985, Astrophys. J. 290, 185.CrossRefGoogle Scholar
Dorland, H. et al.: 1986, Astron. Astrophys. in press.Google Scholar
Gray, D.R., Kilkenny, J.D.: 1980, Plasma Phys. 22, 81.CrossRefGoogle Scholar
Kwitter, K.B.: 1981, Astrophys. J. 245, 154.CrossRefGoogle Scholar
Leahy, D.A.: 1985, Monthly Notices Roy. Astron. Soc. 217, 69.CrossRefGoogle Scholar
Luciani, J.F. et al.: Phys. Rev. Lett. 51, 1664.CrossRefGoogle Scholar
Luciani, J.F.: 1985, Phys. Fluids 28, 835.CrossRefGoogle Scholar
Seward, F.D., and Chlebowski, T.: 1982, Astrophys. J. 256, 530.CrossRefGoogle Scholar
Turner, B.E., and Matthews, H.E.: 1984, Astrophys. J. 277, 164.CrossRefGoogle Scholar
Weaver, R. et al.: 1977, Astrophys. J. 218, 377.CrossRefGoogle Scholar