  A mapping survey towards 51 Planck cold clumps projected on Orion complex was
performed with J=1-0 lines of $^{12}$CO and $^{13}$CO at the 13.7 m telescope
of Purple Mountain Observatory. The mean column densities of the Planck gas
clumps 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 temperatures
of these clumps range from 7.4 to 21.1 K, with an average value of 12.1$\pm$3.0
K. The averaged three-dimensional velocity dispersion $\sigma_{3D}$ in these
molecular 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 lines
correlates with the aperture flux at 857 GHz of the dust emission. Through
analyzing the distributions of the physical parameters, we suggest turbulent
flows can shape the clump structure and dominate their density distribution in
large scale, but not affect in small scale due to the local fluctuations.
Eighty two dense cores are identified in the molecular clumps. The dense cores
have 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 more
affected by turbulence, while those of high column density cores are more
concerned by other factors, especially by gravity. The correlation of the
velocity dispersion versus core size is very weak for the dense cores. The
dense cores are found most likely gravitationally bounded rather than pressure
confined. The relationship between $M_{vir}$ and $M_{LTE}$ can be well fitted
with a power law. The core mass function here is much more flatten than the
stellar initial mass function. The lognormal behavior of the core mass
distribution is most likely determined by the internal turbulence.
