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Triggered star formation in the Magellanic Clouds

Published online by Cambridge University Press:  01 August 2006

Kenji Bekki*
Affiliation:
School of Physics, University of New South Wales, Sydney 2052, Australia email: bekki@phys.unsw.edu.au
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Abstract

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We discuss how tidal interaction between the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), and the Galaxy triggers galaxy-wide star formation in the Clouds for the last ~0.2 Gyr based on our chemodynamical simulations on the Clouds. Our simulations demonstrate that the tidal interaction induces the formation of asymmetric spiral arms with high gas densities and consequently triggers star formation within the arms in the LMC. Star formation rate in the present LMC is significantly enhanced just above the eastern edge of the LMC's stellar bar owing to the tidal interaction. The location of the enhanced star formation is very similar to the observed location of 30 Doradus, which suggests that the formation of 30 Doradus is closely associated with the last Magellanic collision about 0.2 Gyr ago. The tidal interaction can dramatically compress gas initially within the outer part of the SMC so that new stars can be formed from the gas to become intergalactic young stars in the inter-Cloud region (e.g., the Magellanic Bridge). The metallicity distribution function of the newly formed stars in the Magellanic Bridge has a peak of [Fe/H] ~−0.8, which is significantly lower than the stellar metallicity of the SMC.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

Bekki, K. & Chiba, M. 2005, MNRAS 356, 680CrossRefGoogle Scholar
Bekki, K. & Chiba, M. 2006, ApJ (Letters), submittedGoogle Scholar
Bekki, K., Couch, W. J., Beasley, M. A., Forbes, D. A., Chiba, M. & Da Costa, G. S. 2004, ApJ 610, L93CrossRefGoogle Scholar
Fukui, Y., et al. 1999, PASJ 51, 745CrossRefGoogle Scholar
Girardi, L., Chiosi, C., Bertelli, G. & Bressan, A. 1995, A&A 298, 87Google Scholar
Grebel, E. K. & Brandner, W. 1998, in: Richtler, T. & Braun, J.M. (eds.), The Magellanic Clouds and Other Dwarf Galaxies (Aachen, Shaker Verlag), p. 151Google Scholar
Kennicutt, R. C., Jr. 1998, ARAA 36, 189CrossRefGoogle Scholar
Mizuno, N., Muller, E., Maeda, H., Kawamura, A., Minamidani, T., Onishi, T., Mizuno, A. & Fukui, Y. 2006, ApJ 643, L107CrossRefGoogle Scholar
Staveley-Smith, L.Kim, S., Calabretta, M. R., Haynes, R. F. & Kesteven, M. J. 2003, MNRAS 339, 87CrossRefGoogle Scholar
Westerlund, B. E. 1997, The Magellanic Clouds (Cambridge: Cambridge Univ.)CrossRefGoogle Scholar