  We develop a statistical approach for description of dense structures (cores)
in molecular clouds that might be progenitors of stars. Our basic assumptions
are a core mass-density relationship and a power-law density distribution of
these objects as testified by numerical simulations and observations. The core
mass function (CMF) was derived and its slope in the high-mass regime was
obtained analytically. Comparisons with observational CMFs in several Galactic
clouds are briefly presented.
