Titlebook: Dynamics of Star Clusters; Proceeding of the 11 Jeremy Goodman,Piet Hut Conference proceedings 1985 International Astronomical Union 1985 C

縮短

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Systemic

https://doi.org/10.1007/978-1-349-08314-5ion of which is often bimodal. An archetype example of this phenomenon is NGC 6752 (Norris et al. 1981). As documented by Da Costa and Cottrell (1980), and Norris et al. (1981), the CN-rich giants in this cluster possess enhancements in nitrogen abundance by factors of 7–8 relative to the CN-poor gi

adj憂郁的

https://doi.org/10.1007/978-1-349-08390-9o modify the system so that it approaches a more probable configuration. In statistical equilibrium, the distribution of stars among states of different energy, E., per unit mass would be determined to a first approximation by the probability P., where . here g. is the statistical weight of each sta

控制

https://doi.org/10.1007/978-1-349-08390-9of the models of Hénon, Goodman, and Inagaki and Lynden-Bell, as well as evaporative models, and modifications to these models which are needed in the core. Next, these models are related to more detailed numerical calculations of gaseous models, Fokker-Planck models, N-body calculations, etc., and

緯線

A Search for Post-Collapse Coresd, and two possible candidates. The estimated fraction of clusters with this core morphology in the Galaxy is only a few percent. Most clusters do not show a morphology similar to the predictions of the central black hole models.

冰河期

Where’s the CUSP? (Or CCD Photometry of Globular Cluster Cores)part of a major study of globular cluster core structure. These data are being used to test for the presence of central cusps in the surface brightness profiles; which are expected to be present in clusters which have already undergone core collapse (Cohn and Hut 1984).

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Rotational Field and Velocity Dispersion in Globular Clusters: ω Cen and 47 Tucrom the centre to the edge and the ordered to random motions ratios are deduced for two globular clusters: ω Cen and 47 Tuc. Masses through virial theorem and M/L ratios are also given. A more comprehensive study will be published in Astron. & Astrophys.

fleeting

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