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Comparison between Simulations and Theory: where we stand

Published online by Cambridge University Press:  27 April 2011

Joe J. Monaghan
Joe J. Monaghan*
Affiliation:
School of Mathematical Sciences, Vic 3800, Monash University, Australia email: joe.monaghan@monash.edu
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Abstract

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In this paper I relate progress in the simulation of star formation to a remarkable early (1962) paper by Fowler and Hoyle who analyzed star formation in terms of the relevant energies starting from the formation of a large (100 pc) cloud and ending with the final mass distribution of the stars. The way in which modern simulations have clarified and corrected the Fowler-Hoyle picture, and areas where we could improve our simulations, are discussed.

Keywords

Star formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 521 - 526
Copyright
Copyright © International Astronomical Union 2011

References

Clercx, H. H., Nielson, A. H., Torres, D. J., & Coutsias, E. A. 2001, Euro. J. Mech-B/Fluids, 20, 557CrossRefGoogle Scholar
Fowler, W. A. & Hoyle, F. 1962, Roy. Obs. Bulletins. Her Majesty's Stationary Office., Number 67Google Scholar
Grenier, N., Antuono, M., Colagrossi, A., LeTouzé, D., & Alessandrini, B. 2009, J. Computat. Phys, 228, 8380CrossRefGoogle Scholar
Monaghan, J. J. 2005, Rep. Prog. Phys., 68, 1703CrossRefGoogle Scholar