Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-23T15:27:18.485Z Has data issue: false hasContentIssue false
  • English
  • Français

NANTEN observations of triggered star formation: from H II regions to galaxy collisions

Published online by Cambridge University Press:  01 August 2006

N. Mizuno ,
A. Kawamura ,
T. Onishi ,
A. Mizuno  and
Y. Fukui
N. Mizuno
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, JAPAN email: [email protected]
A. Kawamura
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, JAPAN email: [email protected]
T. Onishi
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, JAPAN email: [email protected]
A. Mizuno
Affiliation:
Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, JAPAN
Y. Fukui
Affiliation:
Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, JAPAN email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

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.

In this contribution, we will overview the NANTEN observations of molecular clouds faced to H II regions, supershells, and interacting galaxies, which demonstrate that star/molecular cloud formation is being triggered by young OB associations, supershells, and collisions between galaxies. The large volume filling factor of explosive events like supernovae, ultraviolet radiation fields and stellar winds of massive stars suggest that most of the interstellar medium has been agitated by such strong impacts and triggered star formation is a common event at all scales from small molecular clouds to large galaxy-galaxy mergers. The consequence is the increase of star formation efficiency in many cases, and that more massive stars or clusters of more member stars tend to be formed by triggering than in spontaneous star formation.

Keywords

stars: formationISM: bubblesISM: cloudsradio lines: ISMMagellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 128 - 131
Copyright
Copyright © International Astronomical Union 2007

References

Dawson, J. et al. 2006, this volumeGoogle Scholar
Fukui, Y. et al. 1999, PASJ 51, 751CrossRefGoogle Scholar
Fukui, Y. 2006, this volumeGoogle Scholar
Hartmann, D., & Burton, W. B. 1997, Atlas of Galactic Neutral Hydrogen, (Cambridge: Cambridge University Press)Google Scholar
Kawamura, A. et al. 2006, this volumeGoogle Scholar
Kun, M. et al. 2001, PASJ 53, 1063CrossRefGoogle Scholar
Massey, P., Johnson, K. E., & Degioia-Eastwood, K. 1995, ApJ 454, 151Google Scholar
Matsunaga, K. et al. 2001, PASJ 53, 1003CrossRefGoogle Scholar
McKee, C. F., & Williams, J. P. 1997, ApJ 476, 144CrossRefGoogle Scholar
Mizuno, N., Muller, E., Maeda, H., Kawamura, A., Minamidani, T., Onishi, T., Mizuno, A., & Fukui, Y. 2006, Ap. Lett. 643, 107CrossRefGoogle Scholar
Palouš, J., & Ehlerova, S. 2000, New Astron. Rev 44, 363CrossRefGoogle Scholar
Yamaguchi, R. et al. 1999, PASJ 51, 791CrossRefGoogle Scholar