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We have analyzed HCN(1-0) and CS(2-1) line profiles obtained with highsignal-to-noise ratios toward distinct positions in three selected objects inorder to search for small-scale structure in molecular cloud cores associatedwith regions of high-mass star formation. In some cases, ripples were detectedin the line profiles, which could be due to the presence of a large number ofunresolved small clumps in the telescope beam. The number of clumps for regionswith linear scales of ~0.2-0.5 pc is determined using an analytical model anddetailed calculations for a clumpy cloud model; this number varies in therange: ~2 10^4-3 10^5, depending on the source. The clump densities range from~3 10^5-10^6 cm^{-3}, and the sizes and volume filling factors of the clumpsare ~(1-3) 10^{-3} pc and ~0.03-0.12. The clumps are surrounded by inter-clumpgas with densities not lower than ~(2-7) 10^4 cm^{-3}. The internal thermalenergy of the gas in the model clumps is much higher than their gravitationalenergy. Their mean lifetimes can depend on the inter-clump collisional rates,and vary in the range ~10^4-10^5 yr. These structures are probably connectedwith density fluctuations due to turbulence in high-mass star-forming regions.

A Search for Small-Scale Clumpiness in Dense Cores of Molecular Clouds