Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-24T02:15:05.016Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation of Giant Molecular Clouds by Coagulation of Small Molecular Clouds in a Spiral Gravitational Potential

Published online by Cambridge University Press:  04 August 2017

Kohji Tomisaka
Kohji Tomisaka*
Affiliation:
Department of Physics, Hokkaido University, Sapporo 060, Japan

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.

The formation process of giant molecular clouds (GMCs) is investigated from the standpoint of the coagulation theory of molecular clouds. Small clouds collide with each other and grow to become massive ones. Ultimately they form GMCs with a finite lifetime. The occurrence of star formation in a GMC destroys it and consequently small clouds are formed again. We study the time evolution of the clouds which move through a spiral gravitational potential by an N-body simulation. Then the ensemble of clouds responds to the spiral potential and forms a spiral structure similar to that produced by hydrodynamical galactic shock. It is shown that GMCs are formed in the spiral arm region by collisions between clouds. The distribution of GMCs indicates their short lifetime, of the order of a few times 107 years.

Type
II. Large Scale Processes of Star Formation
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 541 - 543
Copyright
Copyright © Reidel 1987 

References

Sanders, D.B., Scoville, N.Z., & Solomon, P.M. 1985, Ap. J., 289, 373.CrossRefGoogle Scholar
Solomon, P.M., Sanders, D.B., & Rivolo, A.R. 1985, Ap. J. (Letters), 292, L19.Google Scholar
Tomisaka, K. 1984, Publ. Astron. Soc. Japan, 35, 457 (Paper I).Google Scholar
Tomisaka, K. 1986, Publ. Astron. Soc. Japan, 36, 95 (Paper II).Google Scholar