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Star formation in the solar neighbourhood

Published online by Cambridge University Press:  13 January 2020

Mika Juvela Open the ORCID record for Mika Juvela [Opens in a new window]
Mika Juvela*
Affiliation:
Department of physics, University of Helsinki, P.O. Box 64 (Gustaf Hällströmin katu 2), FI-00014 University of Helsinki, Finland email: [email protected]
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Abstract

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Star formation started as a cosmic process soon after the big bang and still continues in the Milky Way, although at a decreasing rate. The formation of dense interstellar clouds, their fragmentation and eventual collapse lead to the birth of stars. The nearby clouds provide the highest resolution for the study of this process. The progress is closely following the improvement of the infrared and radio-wavelength facilities that enables us to follow even the earliest stages of the star-formation process inside molecular clouds. On the other hand, modern numerical simulations can take into account most of the relevant physics and often provide a more direct access into the general principles of star formation. The comparison of observations and simulations is therefore essential. In this paper, will discuss star formation in the solar neighbourhood, concentrating on the prestellar phases leading up to the formation of protostars.

Keywords

stars: formationISM: cloudsISM: kinematics and dynamicsISM: structureISM: magnetic fieldsdustextinctioninfrared: ISMradio lines: ISMsubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 15 - 22
Copyright
© International Astronomical Union 2020 

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