  Polarimeric maps have been used on the characterization of the magnetic field
in molecular clouds. However, it is difficult to determine the 3-dimensional
properties of these regions from the projected maps. In that case, numerical
simulations can be used as benchmarks for polarimetric measurements, and
evetually reveal more about the interplay of turbulence and the magnetic field
lines. In this work we provide a number of MHD numerical simulations of
turbulent molecular clouds and created their synthetic dust emission
polarization maps, varying the direction of the observer. We determined the
correlation of emission intensity and polarization degree for the simulated
models. We were able to reproduce the decay on polarization degree at denser
regions without any assumption regarding the properties of the dusty component.
The anti-correlation arises from the simple cancelation of the polarization
vectors along the line of sight. This effect is amplified within denser regions
as the magnetic field configuration becomes more complex. We studied the
probability distribution, the power spectrum and the structure function of the
polarization angles. These statistical analysis revealed strong defferences
depending on the turbulent regime (i.e. sub/supersonic and sub/super-Alfvenic).
Therefore, these methods can be used on polarimetric observations to
characterize the dynamics of molecular clouds. We also presented a modified
Chandrashekhar-Fermi method to obtain the intensity of the local magnetic
field. The proposed formulation showed no limitations regarding orientation or
turbulent regime.
