Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-25T23:50:23.490Z Has data issue: false hasContentIssue false
  • English
  • Français

Numerical simulation of star formation in filamentary dark molecular clouds

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

Published online by Cambridge University Press:  12 September 2016

Pak Shing Li ,
Richard I. Klein  and
Christopher F. McKee
Pak Shing Li
Affiliation:
Astronomy Department, University of California, 501 Campbell Hall #3411, Berkeley, CA 94720-3411, USA email: [email protected]
Richard I. Klein
Affiliation:
Astronomy Department, University of California, 501 Campbell Hall #3411, Berkeley, CA 94720-3411, USA email: [email protected] Lawrence Livermore National Laboratory, P.O. Box 808, L-23, Livermore, CA 94550, USA, email: [email protected]
Christopher F. McKee
Affiliation:
Astronomy Department, University of California, 501 Campbell Hall #3411, Berkeley, CA 94720-3411, USA email: [email protected] Physics Department, University of California, Berkeley, CA 94720, USA, email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Numerical simulations of star formation faces challenges including the huge spatial dynamic range and the presence of multiply coupled highly non-linear physics, such as magnetic field, supersonic turbulence, gravitation, radiation and protostellar outflow feedback. We present in this symposium our latest high resolution adaptive mesh refinement numerical simulations of the formation of filamentary dark molecular clouds from 4.55 pc size scale down to the formation of a protostellar cluster with maximum resolution at 28 AU. The physical properties of the long braided filamentary dark cloud formed in the simulation, the magnetic field properties of the cloud clumps, and the protostellar mass function in the simulations match well with the latest observations.

Keywords

Magnetic fields-MHD-ISM: magnetic fields-ISM: kinematics and dynamics- stars: 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. 103 - 106
Copyright
Copyright © International Astronomical Union 2016 

References

Chabrier, G. 2005, in: Corbelli, E. & Palla, F. (eds.), The Initial Mass Function 50 Years Later Ap&SSL Conf. Ser., 327, 41 Google Scholar
Crutcher, R. M., Wandelt, B., Heiles, C., Falgarone, E., & Troland, T. H. 2010, ApJ, 725, 466 Google Scholar
Li, H.-b., Dowell, C. D., Goodman, A., Hildebrand, R., & Novak, G. 2009, ApJ, 704, 891 Google Scholar
Li, P. S., Martin, D. F., Klein, R. I., & McKee, C. F. 2012, ApJ, 745, 139 Google Scholar
Li, P. S., McKee, C. F., & Klein, R. I. 2015a, MNRAS, 30, 490 Google Scholar
Li, P. S., Klein, R. I., & McKee, C. F. 2015b, in preparationGoogle Scholar
Li, P. S., Klein, R. I., & McKee, C. F. 2016, in preparationGoogle Scholar
McKee, C. F. & Offner, S. S. R. 2010, ApJ, 716, 167 Google Scholar
Peretto, N., Fuller, G. A., André, Ph., et al. 2014, A&A, 561, A83 Google Scholar