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Pre–Main Sequence Evolution of Star Forming Regions and Young Clusters

Published online by Cambridge University Press:  16 November 2011

C. Charbonnel ,
T. Montmerle  and
F. Palla
F. Palla*
Affiliation:
INAF-Osservatorio Astrofisico di Arcetri, L.go E. Fermi, 5, 50125 Firenze, Italy
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Abstract

This review covers a variety of topics related to the properties of Pre–Main Sequence stars in star forming regions, young clusters and associations. Some recent developments of theoretical models of PMS evolution are discussed, with emphasis on the role of magnetic fields in low-mass stars and their impact on observable quantities. Critical tests on the comparison between model predictions and observations are presented for stars across the mass spectrum. The issue of the formation and early evolution of massive stars is addressed, with emphasis on clustered versus isolated objects. After a brief historical background on the derivation of the Initial Mass Function, current representations of this quantity are discussed. The issue of the duration of the star formation process is dealt with using the results of age dating methods for young stars, mainly based on the property of Lithium depletion during PMS evolution. A recent analysis of the properties of the stellar population of the Orion Nebula Cluster is presented with the resulting IMF and age distributions. Finally, a discussion of recent determinations of the metallicity distribution of young stars in clusters and associations closes the review.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 51: Star Formation in the Local Universe – EES2010 , 2011 , pp. 245 - 287
Copyright
© EAS, EDP Sciences, 2011

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