缩短 发表于 2025-3-28 18:40:20
http://reply.papertrans.cn/29/2842/284181/284181_41.pngheckle 发表于 2025-3-28 21:14:16
http://reply.papertrans.cn/29/2842/284181/284181_42.pngSystemic 发表于 2025-3-28 23:19:50
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 giadj忧郁的 发表于 2025-3-29 05:17:44
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 发表于 2025-3-29 09:48:47
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纬线 发表于 2025-3-29 13:22:06
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 发表于 2025-3-29 18:56:17
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).消毒 发表于 2025-3-29 23:20:39
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 发表于 2025-3-30 00:40:25
http://reply.papertrans.cn/29/2842/284181/284181_49.png钢盔 发表于 2025-3-30 06:14:17
http://reply.papertrans.cn/29/2842/284181/284181_50.png