Self-similar solutions for post-collapse evolution of globular clusters

Details Self-similar solutions for post-collapse evolution of globular clusters Self-similar solutions for post-collapse evolution of globular clusters

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.205..913i&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 205, Dec. 1983, p. 913-930. Research supported by the J

Astronomy and Astrophysics

Astrophysics

63

Astrophysics, Fokker-Planck Equation, Globular Clusters, Stellar Evolution, Astronomical Models, Asymptotic Methods, Binary Stars, Stellar Mass

Scientific paper

Evolution under the Fokker-Planck equation predicts that the central densities of globular clusters will become infinite in finite time with density profiles ρ ∝ r-α at that moment (and α ≅ 2.21). The dynamical evolution of the cores after that time, t0, is predicted here. The re-expansion of the cluster is powered by the energy released due to binary formation at the centre. This is modelled, following Hénon, as a point energy source. That much can be deduced from general principles; detailed spatial profiles require a computation. Following Hachisu et al. these are computed for the conductive gas model.

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