Radial density profiles for the sample of dense cores associated with high-mass star-forming regions from southern hemisphere have been derived using the data of observations in continuum at 250Â GHz .
Radial density profiles for the inner regions of 16 cores ( at distances \la 0.2 - 0.8 Â pc from the center ) are close on average to the \rho \propto r ^ { - \alpha } dependence , where \alpha = 1.6 \pm 0.3 .
In the outer regions density drops steeper .
An analysis with various hydrostatic models showed that the modified Bonnor-Ebert model , which describes turbulent sphere confined by external pressure , is preferable compared with the logotrope and polytrope models practically in all cases .
With a help of the Bonnor-Ebert model , estimates of central density in a core , non-thermal velocity dispersion and core size are obtained .
The comparison of central densities with the densities derived earlier from the CS modeling reveals differences in several cases .
The reasons of such differences are probably connected with the presence of density inhomogenities on the scales smaller than the telescope beam .
In most cases non-thermal velocity dispersions are in agreement with the values obtained from molecular line observations .