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Star Formation Thresholds

Published online by Cambridge University Press:  01 June 2007

Joop Schaye
Joop Schaye*
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, the Netherlands email: [email protected]
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Abstract

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To make predictions for the existence of “dark galaxies”, it is necessary to understand what determines whether a gas cloud will form stars. Star formation thresholds are generally explained in terms of the Toomre criterion for gravitational instability. I contrast this theory with the thermo-gravitational instability hypothesis of Schaye (2004), in which star formation is triggered by the formation of a cold gas phase and which predicts a nearly constant surface density threshold. I argue that although the Toomre analysis is useful for the global stability of disc galaxies, it relies on assumptions that break down in the outer regions, where star formation thresholds are observed. The thermo-gravitational instability hypothesis can account for a number of observed phenomena, some of which were thought to be unrelated to star formation thresholds.

Keywords

stars: formationISM: structuregalaxies: formationgalaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 247 - 255
Copyright
Copyright © International Astronomical Union 2008

References

Auld, R., de Blok, W. J. G., Bell, E. & Davies, J. I. 2006, MNRAS, 366, 1475CrossRefGoogle Scholar
Braun, R. 1997, ApJ, 484, 637CrossRefGoogle Scholar
de Blok, W. J. G. & Walter, F., 2006, AJ, 131, 363CrossRefGoogle Scholar
Elmegreen, B. G. & Parravano, A. 1994, ApJ, 435, L121CrossRefGoogle Scholar
Ferguson, A. M. N., Wyse, R. F. G., Gallagher, J. S. & Hunter, D. A. 1998, ApJ, 506, L19CrossRefGoogle Scholar
Ferland, G. J. 2000, Revista Mexicana de Astronomia y Astrofisica Conference Series, 9, 153Google Scholar
Guiderdoni, B., 1987, A&A, 172, 27Google Scholar
Hunter, D. A., Elmegreen, B. G. & Baker, A. L. 1998, ApJ, 493, 595CrossRefGoogle Scholar
Kennicutt, R. C. 1989, ApJ, 344, 685CrossRefGoogle Scholar
Lo, K. Y., Sargent, W. L. W. & Young, K. 1993, AJ, 106, 507CrossRefGoogle Scholar
Martin, C. L. & Kennicutt, R. C. 2001, ApJ, 555, 301 (MK01)CrossRefGoogle Scholar
Maybhate, A., Masiero, J., Hibbard, J. E., Charlton, J. C., Palma, C., Knierman, K. A. & English, J., 2007, arXiv, 707, arXiv:0707.3582Google Scholar
Meurer, G. R., Carignan, C., Beaulieu, S. F. & Freeman, K. C. 1996, AJ, 111, 1551CrossRefGoogle Scholar
Quirk, W. J. 1972, ApJ, 176, L9CrossRefGoogle Scholar
Schaye, J. 2001, ApJ, 562, L95CrossRefGoogle Scholar
Schaye, J. 2004, ApJ, 609, 667 (S04)CrossRefGoogle Scholar
Sellwood, J. A. & Balbus, S. A. 1999, ApJ, 511, 660CrossRefGoogle Scholar
Skillman, E. D. 1987, in Star Formation in Galaxies, edited by Persson, C. J. Londsdale (NASA Conf. Pub. CP-2466), p. 263Google Scholar
Taylor, C. L., Brinks, E., Pogge, R. W. & Skillman, E. D. 1994, AJ, 107, 971CrossRefGoogle Scholar
Wada, K., Meurer, G. & Norman, C. A. 2002, ApJ, 577, 197CrossRefGoogle Scholar
Wong, T. & Blitz, L. 2002, ApJ, 569, 157CrossRefGoogle Scholar