Hostname: page-component-7bb8b95d7b-dtkg6 Total loading time: 0 Render date: 2024-10-04T01:16:36.720Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of Zero-Metal Clouds

Published online by Cambridge University Press:  04 August 2017

K. R. Villere  and
P. H. Bodenheimer
K. R. Villere
Affiliation:
Board of Studies in Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA
P. H. Bodenheimer
Affiliation:
Board of Studies in Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA

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.

Dynamical, chemical and thermal evolution of zero-metal gas clouds has been modeled to study conditions of star formation in the early universe. Numerical results are shown for collapse of a spherical cloud of mass 5 × 105 M⊙. Cooling by H2 lines and by photons emitted in H + e- → H- + hν maintains collapse until formation of an equilibrium protostellar core with mass 0.03 M⊙. the cooling by photons produced with H- is essential for low-mass star formation. If the cloud is fragmented, the evolution of each piece resembles that of the parent cloud.

Type
Early Universe
Information
Symposium - International Astronomical Union , Volume 120: Astrochemistry , 1987 , pp. 121 - 122
Copyright
Copyright © Reidel 1987 

References

Bodenheimer, P. 1968, Ap. J., 153, 483.Google Scholar
Palla, F., Salpeter, E.E., and Stahler, S.W. 1983, Ap. J., 271, 632.Google Scholar
Stahler, S.W., Palla, P., and Salpeter, E.E. 1985, preprint.Google Scholar