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

Corrugate

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

不持續(xù)就爆

Affectation

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

arrhythmic

艦旗

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.

DECRY

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

DECRY

nurture

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.

先兆

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

脊椎動(dòng)物

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,