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Molecular cloud fragmentation and core collapse

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Shantanu Basu
Shantanu Basu*
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario N6A 3K7, Canada email: basu@uwo.ca
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Abstract

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I review some steps in the conversion of molecular cloud gas into stars and planets, with an emphasis in this presentation on the early stage molecular cloud fragmentation that leads to elongated filaments/ribbons. Magnetic fields can play a crucial role in all stages and need to be invoked particularly for early stage fragmentation as well as in late core collapse where it may control disk formation. I also review some elements of hydrodynamic modeling of disk evolution.

Keywords

ISM: cloudsISM: magnetic fieldsISM: moleculesMHDstars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , pp. 85 - 90
Copyright
Copyright © International Astronomical Union 2016 

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