Finding out the velocity anisotropy parameter for some globular clusters: the case of stationary model
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The problem of determination of the velocity anisotropy parameter (A) from star density profiles in globular clusters is considered. The calculations are performed for following clusters: M3, M12, M13, M15, M55, M56, Palomar 3, Palomar 14, NGC5139 (Omega Centauri) and NGC6535. We found that for most clusters is A=0. For M56 the parameter is calculated at limiting magnitudes B=21.5 and B=19.0 and we found A=0.8 and A=0.3 respectively. For Omega Centauri the anisotropy parameter is determined in three separate regions and we found: A=0 for central region, A=0.1 for middle region and A=0.3 for halo.
3 pages, no figures, LaTeX, submitted to "Dynamics of Star Clusters and the Milky Way" eds S. Deiters, B. Fuchs, A. Just, R. Spurzem, and R. Wielen
3 pages, no figures, LaTeX, submitted to "Dynamics of Star Clusters and the Milky Way" eds S. Deiters, B. Fuchs, A. Just, R. Spurzem, and R. Wielen