  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.
