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Heating of stellar disks by massive gas clouds

Published online by Cambridge University Press:  04 August 2017

Cedric G. Lacey
Cedric G. Lacey*
Affiliation:
Institute of Astronomy, Cambridge, England

Extract

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I have analytically calculated the evolution of the three components of velocity dispersion of the stars in a galactic disk when these are scattered by massive gas clouds, in a generalization of Spitzer & Schwarzschild's (1953) calculation. The principal assumptions made are: (i) The stellar orbits obey the epicyclic approximation. (ii) The gas clouds are massive, long-lived and on circular orbits. (iii) The typical star-cloud encounter time is short compared to the orbital time. (iv) The evolution due to encounters is treated as a diffusion process.

Type
PART III: Dynamics and Evolution
Information
Symposium - International Astronomical Union , Volume 106: The Milky Way Galaxy , 1985 , pp. 493 - 496
Copyright
Copyright © Reidel 1985 

References

Chandrasekhar, S. 1960, “Principles of Stellar Dynamics” (Dover).Google Scholar
Lacey, C.G. 1984, Mon. Not. R. astron. Soc., in press.Google Scholar
Spitzer, L. and Schwarzschild, M. 1953, Astrophys. J. 118, p. 306.Google Scholar
van der Kruit, P.C. and Searle, L. 1981, Astron. Astrophys. 95, p. 105.Google Scholar
Wielen, R. 1974, Highlights of Astronomy 3 (Dordrecht: Reidel), p. 395.Google Scholar