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Why are Stellar Systems Anisotropic?

Published online by Cambridge University Press:  04 August 2017

E. Bettwieser ,
K. J. Fricke  and
R. Spurzem
E. Bettwieser
Affiliation:
Universitätssternwarte, Geismarlandstraβe 11, D-3400 Göttingen, Federal Republic of Germany
K. J. Fricke
Affiliation:
Universitätssternwarte, Geismarlandstraβe 11, D-3400 Göttingen, Federal Republic of Germany
R. Spurzem
Affiliation:
Universitätssternwarte, Geismarlandstraβe 11, D-3400 Göttingen, Federal Republic of Germany

Extract

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Spherical stellar systems show during their secular evolution the development of velocity anisotropy in their halo (cf. e.g. Hénon, 1971). The present study examines the general reasons for generation of anisotropy in stellar systems by means of a gaseous star cluster model including anisotropy. Moment equations of the Boltzmann equation are considered for spherical symmetry in coordinate space but not in velocity space closed in third order by a heat flux equation. The coefficient of heat conductivity is tailored to describe the flux of energy due to the cumulative effect of distant gravitative encounters and generalized to include effects of anisotropy and external gravitation by a massive central object (Bettwieser et al., 1984).

Type
May 30: Model System in the Point-Mass Approximation
Information
Symposium - International Astronomical Union , Volume 113: Dynamic of Stars Clusters , 1985 , pp. 301 - 303
Copyright
Copyright © Reidel 1985 

References

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