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A mapping survey towards 51 Planck cold clumps projected on Orion complex wasperformed with J=1-0 lines of $^{12}$CO and $^{13}$CO at the 13.7 m telescopeof Purple Mountain Observatory. The mean column densities of the Planck gasclumps range from 0.5 to 9.5$\times10^{21}$ cm$^{-2}$, with an average value of(2.9$\pm$1.9)$\times10^{21}$ cm$^{-2}$. While the mean excitation temperaturesof these clumps range from 7.4 to 21.1 K, with an average value of 12.1$\pm$3.0K. The averaged three-dimensional velocity dispersion $\sigma_{3D}$ in thesemolecular clumps is 0.66$\pm$0.24 km s$^{-1}$. Most of the clumps have$\sigma_{NT}$ larger than or comparable with $\sigma_{Therm}$. The H$_{2}$column density of the molecular clumps calculated from molecular linescorrelates with the aperture flux at 857 GHz of the dust emission. Throughanalyzing the distributions of the physical parameters, we suggest turbulentflows can shape the clump structure and dominate their density distribution inlarge scale, but not affect in small scale due to the local fluctuations.Eighty two dense cores are identified in the molecular clumps. The dense coreshave an averaged radius and LTE mass of 0.34$\pm$0.14 pc and 38$_{-30}^{+5}$M$_{\sun}$, respectively. And structures of low column density cores are moreaffected by turbulence, while those of high column density cores are moreconcerned by other factors, especially by gravity. The correlation of thevelocity dispersion versus core size is very weak for the dense cores. Thedense cores are found most likely gravitationally bounded rather than pressureconfined. The relationship between $M_{vir}$ and $M_{LTE}$ can be well fittedwith a power law. The core mass function here is much more flatten than thestellar initial mass function. The lognormal behavior of the core massdistribution is most likely determined by the internal turbulence.

Molecular environments of 51 Planck cold clumps in Orion complex