標(biāo)題: Titlebook: Dynamics of Star Clusters; Proceeding of the 11 Jeremy Goodman,Piet Hut Conference proceedings 1985 International Astronomical Union 1985 C [打印本頁] 作者: Corrugate 時(shí)間: 2025-3-21 16:07
書目名稱Dynamics of Star Clusters影響因子(影響力)
書目名稱Dynamics of Star Clusters影響因子(影響力)學(xué)科排名
書目名稱Dynamics of Star Clusters網(wǎng)絡(luò)公開度
書目名稱Dynamics of Star Clusters網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Dynamics of Star Clusters被引頻次
書目名稱Dynamics of Star Clusters被引頻次學(xué)科排名
書目名稱Dynamics of Star Clusters年度引用
書目名稱Dynamics of Star Clusters年度引用學(xué)科排名
書目名稱Dynamics of Star Clusters讀者反饋
書目名稱Dynamics of Star Clusters讀者反饋學(xué)科排名
作者: 不持續(xù)就爆 時(shí)間: 2025-3-21 23:48 作者: Affectation 時(shí)間: 2025-3-22 03:41
A High Spatial Resolution Investigation of the Core of Some Dynamically Evolved Globular Clusterses reaches 0.5 on the best plates). Good plates of M 79, M 53, M 3, M 5, M 13, M 92, NGC 6397, M 15, M 2 and M 30 were obtained (Aurière and Cordoni, 1983, Astron. Astrophys. Suppl. Ser. ., 383 and references therein). The observations are mainly obtained at the 2 m and 1 m Cassegrain telescopes of 作者: arrhythmic 時(shí)間: 2025-3-22 06:33 作者: 艦旗 時(shí)間: 2025-3-22 12:12
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.作者: DECRY 時(shí)間: 2025-3-22 14:09
Observed Dynamical Parameters of Star Clusters in the SMCopen clusters whereas the “halo” red clusters are less massive and younger than the galactic globulars (Kontizas, Danezis, Kontizas, 1982; Kontizas and Kontizas, 1983). (b) All clusters show density profiles that fit the available theoretical models (King, 1962) giving evidence of relaxed systems, e作者: DECRY 時(shí)間: 2025-3-22 19:48 作者: nurture 時(shí)間: 2025-3-22 21:25
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.作者: 先兆 時(shí)間: 2025-3-23 04:33
BV Concentric Aperture Photometry of Globular Clustersto measurement error are the centering of apertures in the oftentimes diffuse cores of clusters, the random distribution of bright stars near the cluster centers, and the determination of an adequate sky correction in fields badly crowded by foreground stars. These problems have been well-discussed 作者: 脊椎動(dòng)物 時(shí)間: 2025-3-23 08:32
An Extension of the Search for Spectroscopic Binaries in M3a typical accuracy of 0.8 km/s per measurement and have been combined with the Gunn and Griffin data in order to search for radial velocity variations over a time span of ten years. We find no convincing evidence that any of the giants observed are spectroscopic binaries with one notable exception, 作者: chandel 時(shí)間: 2025-3-23 12:28 作者: 潰爛 時(shí)間: 2025-3-23 14:25 作者: Campaign 時(shí)間: 2025-3-23 20:47
Precollapse Evolution of Globular Clusterso 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作者: 巧辦法 時(shí)間: 2025-3-24 01:20 作者: Ballad 時(shí)間: 2025-3-24 04:17 作者: mortuary 時(shí)間: 2025-3-24 09:16 作者: Generic-Drug 時(shí)間: 2025-3-24 13:12
https://doi.org/10.1007/978-1-349-07805-9Proper motion data of Ml3 cluster members are very useful for the investigation of the cluster’s internal dynamics. We introduce a maximum likelihood method to fit these data in terms of conventional King-Michie models.作者: 閃光東本 時(shí)間: 2025-3-24 15:03 作者: 斷言 時(shí)間: 2025-3-24 21:52 作者: Inflamed 時(shí)間: 2025-3-24 23:39 作者: Encephalitis 時(shí)間: 2025-3-25 04:40
Chemical Gradients in Globular ClustersFirst I will describe briefly some older work on chemical gradient in globular clusters. Then I will discuss some more recent data on the chemical and kinematical properties of 47 Tuc and Omega Cen, that leave us in little doubt about the reality of such chemical gradients.作者: Feigned 時(shí)間: 2025-3-25 09:56 作者: 過于光澤 時(shí)間: 2025-3-25 13:05
Core and Tidal Radii of the Carina Dwarf Spheroidal Galaxy from UK Schmidt Telescope PlatesCore and tidal radii of the Carina dwarf galaxy are determined by fitting King dynamical models to number count radial profiles, derived from COSMOS data. These values are compared with those of the other six known Local Group dwarf spheroidals.作者: 牢騷 時(shí)間: 2025-3-25 19:23 作者: 群島 時(shí)間: 2025-3-25 20:14 作者: Vertebra 時(shí)間: 2025-3-26 00:30 作者: CRASS 時(shí)間: 2025-3-26 05:55 作者: Stress-Fracture 時(shí)間: 2025-3-26 11:15 作者: 防御 時(shí)間: 2025-3-26 12:40
International Astronomical Union Symposiahttp://image.papertrans.cn/e/image/284181.jpg作者: 苦澀 時(shí)間: 2025-3-26 17:28
https://doi.org/10.1007/978-94-009-5335-2CCD; Galaxy; black hole; photometry; star; stellar; telescope作者: 真繁榮 時(shí)間: 2025-3-27 01:00 作者: forthy 時(shí)間: 2025-3-27 02:21 作者: 樹膠 時(shí)間: 2025-3-27 08:58 作者: 男生如果明白 時(shí)間: 2025-3-27 11:29 作者: opalescence 時(shí)間: 2025-3-27 17:16 作者: OVER 時(shí)間: 2025-3-27 17:53 作者: convert 時(shí)間: 2025-3-27 23:33
Women in the English Novel, 1800-1900open clusters whereas the “halo” red clusters are less massive and younger than the galactic globulars (Kontizas, Danezis, Kontizas, 1982; Kontizas and Kontizas, 1983). (b) All clusters show density profiles that fit the available theoretical models (King, 1962) giving evidence of relaxed systems, e作者: ineptitude 時(shí)間: 2025-3-28 05:58
https://doi.org/10.1007/978-1-349-08184-4part 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).作者: terazosin 時(shí)間: 2025-3-28 09:54
Von der Schule in die Arbeitsweltrom 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.作者: Lipohypertrophy 時(shí)間: 2025-3-28 13:48 作者: 縮短 時(shí)間: 2025-3-28 18:40 作者: heckle 時(shí)間: 2025-3-28 21:14 作者: Systemic 時(shí)間: 2025-3-28 23:19
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作者: adj憂郁的 時(shí)間: 2025-3-29 05:17
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作者: 控制 時(shí)間: 2025-3-29 09:48
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 作者: 緯線 時(shí)間: 2025-3-29 13:22
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.作者: 冰河期 時(shí)間: 2025-3-29 18:56
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).作者: 消毒 時(shí)間: 2025-3-29 23:20
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.作者: fleeting 時(shí)間: 2025-3-30 00:40 作者: 鋼盔 時(shí)間: 2025-3-30 06:14 作者: 真 時(shí)間: 2025-3-30 09:11 作者: 釋放 時(shí)間: 2025-3-30 14:33
https://doi.org/10.1007/978-1-349-07805-9Pic-du-Midi Observatory. The high spatial resolution of our plates enables us to achieve stellar photometry, at least for the bright stars, in these overcrowded regions. Surface photometry is also obtained.作者: 使高興 時(shí)間: 2025-3-30 16:45
E. J. Neather,Isabelle Rodriguesd giant branch in this cluster (Norris et al., 1984). When combined with the velocities published by the CORAVEL group (Mayor et al., 1983), these observations yield velocities for 212 stars with projected distances from the cluster center ranging from 3 to 68 core radii.作者: IRK 時(shí)間: 2025-3-30 22:05
https://doi.org/10.1007/978-1-349-08390-9some problems for further work in these directions are outlined. The review concludes with a discussion of the relation between theoretical models and observations of the surface density profiles and statistics of actual globular clusters.作者: 爆米花 時(shí)間: 2025-3-31 01:21
1743-9213 posium in the spring of 1984, was the rapid increase during the preceeding year in our understanding of core collapse. The last I.A.D. Symposium to discuss the dynamics of star clusters at length was No.69, Dynamics of Stellar Systems~ held in Besan~on in 1974. For a few years afterwards, globular c作者: CERE 時(shí)間: 2025-3-31 06:32 作者: 哀求 時(shí)間: 2025-3-31 12:06 作者: 蓋他為秘密 時(shí)間: 2025-3-31 14:48
https://doi.org/10.1007/978-1-349-08314-5aries exist in M3 between 4 and 30 core radii from the center. Low luminosity globular X-ray sources could still be weak-lined (E.W. < 12 ?) and bright (M. ? +5 like some old novae) or strong-lined (E.W. ? 60 ?) and faint (M. > 7 like dwarf novae).作者: 較早 時(shí)間: 2025-3-31 17:33
https://doi.org/10.1007/978-1-349-08314-5her the properties of NGC 6752 mentioned above might be consistent with supernova enrichment. Both the free and adiabatic expansion phases of supernova shells (Spitzer 1968) will be discussed in this context.
