Hostname: page-component-7479d7b7d-m9pkr Total loading time: 0 Render date: 2024-07-11T10:25:33.590Z Has data issue: false hasContentIssue false
  • English
  • Français

Equilibrium and Collapse of Rotating Isothermal Clouds

Published online by Cambridge University Press:  04 August 2017

S. Narita ,
M. Kiguchi ,
S. M. Miyama  and
C. Hayashi
S. Narita
Affiliation:
Dept. of, Electronics, Doshisha U., Kyoto 602, Japan
M. Kiguchi
Affiliation:
Inst. of Science and Tech., Kinki U., Osaka 573, Japan
S. M. Miyama
Affiliation:
Dept. of Physics, Kyoto U., Kyoto 606, Japan
C. Hayashi
Affiliation:
Momoyama Yogoro-cho 1, Fushimi-ku, Kyoto 612, Japan

Extract

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.

We have performed numerical calculations for both static and dynamic structures of molecular clouds in which stars would be formed. The assumption in our calculations is that a cloud, which is embedded in an external hot and tenuous uniform medium, is isothermal and axisymmetric.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 377
Copyright
Copyright © Reidel 1987