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Evolutionary sequence of expanding Hydrogen shells

Published online by Cambridge University Press:  01 August 2006

M. Relaño ,
J. E. Beckman ,
O. Daigle  and
C. Carignan
M. Relaño
Affiliation:
Dpto. Física Teórica y del Cosmos, Universidad de Granada, Spain email: [email protected]
J. E. Beckman
Affiliation:
Instituto de Astrofísica de Canarias, C. Vía Láctea s/n, 38200, La Laguna, Tenerife, Spain email: [email protected]
O. Daigle
Affiliation:
Observatoire du mont Mégantic, LAE, Université de Montréal, C. P. 6128 succ. centre ville, Montréal, Québec, CanadaH3C 3J7 email: [email protected], [email protected]
C. Carignan
Affiliation:
Observatoire du mont Mégantic, LAE, Université de Montréal, C. P. 6128 succ. centre ville, Montréal, Québec, CanadaH3C 3J7 email: [email protected], [email protected]
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Abstract

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Giant HI shells, with diameters of hundreds of parsecs and expansion velocities of 10-20 s−1 are characteristic observed features of local gas rich galaxies. Although a predictable consequence of the impact of OB associations on the ISM doubts have been raised, as OB stars are not present in the centres of the majority of these shells. Here we combine our observations of expanding ionized shells in luminous H II regions with basic dynamical models to give support to the scenario in which OB associations do produce the HI shells.

Keywords

galaxiesISM: H II regionskinematics and dynamicsbubbles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 467
Copyright
Copyright © International Astronomical Union 2007

References

Relaño, M. & Beckman, J. E. 2005, A&A 430, 911Google Scholar
Dyson, J.E. 1981 in: Kahn, F. D. (eds.), Investigating the Universe (Dordrecht: Reidel), p. 125CrossRefGoogle Scholar
Hatzidimitriou, D., Stanimirovic, S., Maragoudaki, F., Staveley-Smith, L.Dapergolas, A., & Bratsolis, E. 2005, MNRAS 360, 1171CrossRefGoogle Scholar