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Fokker-Planck Models for Rotating Stellar Systems

Published online by Cambridge University Press:  25 May 2016

Christian Einsel  and
Rainer Spurzem
Christian Einsel
Affiliation:
Institut für Astronomie und Astrophysik der Universität, Olshausenstraße 40, D-24098 Kiel, e-mail: [email protected]
Rainer Spurzem
Affiliation:
Institut für Astronomie und Astrophysik der Universität, Olshausenstraße 40, D-24098 Kiel, e-mail: [email protected]

Extract

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Observations of Globular Cluster ellipticity distributions related to some fundamental parameters give strong evidence for a decay of rotational energy in these systems with time. In order to study the effectiveness of angular momentum transport (or loss, resp.) a code has been written which solves the Fokker-Planck equation in (E, Jz)-space and follows the evolution from some initial conditions through core collapse (and possibly gravothermal oscillations) up to the post-collapse phase. For the purpose of comparability with N-body simulations rotating initial model configurations according to the prescriptions of Lupton & Gunn (1987) have been constructed. These models are intended to continue previous work by Goodman (1983, Fokker-Planck) and Akiyama & Sugimoto (1989, N-Body). In this contribution the derivation of the flux coefficients is given.

Type
Stellar Dynamics, Models
Information
Symposium - International Astronomical Union , Volume 174: Dynamical Evolution of Stars Clusters , 1996 , pp. 363 - 364
Copyright
Copyright © Kluwer 1996 

References

Akiyama, K, Sugimoto, D. 1989, PASJ, 41, 991 Google Scholar
Goodman, J. 1983, , Google Scholar
Lupton, R.H., Gunn, J.E. 1987, AJ, 93, 1106 Google Scholar
Rosenbluth, M.N., MacDonald, W.M., Judd, D.L. 1957, Phys. Rev., 107, 1 Google Scholar
Spitzer, L. jr. 1987, Dynamical Evolution of Globular Clusters, Princeton Univ. Press Google Scholar