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On the structure of giant HII regions and HII galaxies

Published online by Cambridge University Press:  01 August 2006

G. Tenorio-Tagle ,
C. Muñoz-Tuñón ,
E. Pérez ,
S. Silich  and
E. Telles
G. Tenorio-Tagle
Affiliation:
Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla, México email: gtt@inaoep.mx
C. Muñoz-Tuñón
Affiliation:
Instituto de Astrofísica de Canarias, E 38200 La Laguna, Tenerife, Spaincmt@ll.iac.es
E. Pérez
Affiliation:
Instituto de Astrofísica de Andalucía (CSIC), Camino bajo de Huetor 50, E 18080 Granada, Spaineperez@iaa.es
S. Silich
Affiliation:
Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla, México email: gtt@inaoep.mx
E. Telles
Affiliation:
Observatório Nacional, Rua José Cristino 77, 20921-400, Rio de Janeiro, Braziletelles@on.br
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Abstract

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We review the structural properties of giant extragalactic HII regions and HII galaxies based on two dimensional hydrodynamic calculations, and propose an evolutionary sequence that accounts for their observed detailed structure. The model assumes a massive and young stellar cluster surrounded by a large collection of clouds. These are thus exposed to the most important star-formation feedback mechanisms: photoionization and the cluster wind. The models show how the two feedback mechanisms compete with each other in the disruption of clouds and lead to two different hydrodynamic solutions: The storage of clouds into a long lasting ragged shell that inhibits the expansion of the thermalized wind, and the steady filtering of the shocked wind gas through channels carved within the cloud stratum that results into the creation of large-scale superbubbles. Both solutions are here claimed to be concurrently at work in giant HII regions and HII galaxies, causing their detailed inner structure.

Keywords

galaxies: starburst – galaxies: galaxies: HII – galaxies: ISM: HII regions
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 238 - 241
Copyright
Copyright © International Astronomical Union 2007

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