Anisotropic gaseous models for the evolution of star clusters

Details Anisotropic gaseous models for the evolution of star clusters Anisotropic gaseous models for the evolution of star clusters

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.251..408l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 251, Aug. 1, 1991, p. 408-426. Research supported by Un

Astronomy and Astrophysics

Astronomy

46

Star Clusters, Stellar Evolution, Anisotropic Media, Cosmic Gases, Stellar Models

Scientific paper

Two anisotropic gas models for star clusters are presented. Both are extensions of the standard isotropic gas model where the heat flux is proportional to the local temperature gradient and the coefficient of thermal conductivity is a function of the local Jeans length and the local relaxation time. Thy differ in the relation between the third-order moments of the velocity distribution. Self-similar pre-collapse solutions are derived for both models. In both solutions, the power-law index is 2.23 and the ratio of the radial and tangential mean-square velocity dispersion grows to 1.30 in the outer parts of the halo, which is in excellent agreement with higher order fluid-dynamical models including anisotropy.

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