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

真

釋放

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.

使高興

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.

IRK

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.

爆米花

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

CERE

哀求

蓋他為秘密

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).

較早

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.