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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
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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