| Full text | |
| Author(s): |
Falceta-Goncalves, D.
;
Lazarian, A.
;
Kowal, G.
;
Esquivel, A
;
Franco, J
;
GarciaSegura, G
;
DalPino, EMD
;
Lazarian, A
;
Lizano, S
;
Raga, A
Total Authors: 10
|
| Document type: | Journal article |
| Source: | XI IAU REGIONAL LATIN AMERICAN MEETING OF ASTRONOMY; v. 36, p. 2-pg., 2009-01-01. |
| Abstract | |
Polarimetric maps have been used for 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. For that reason, numerical simulations can be used as benchmarks for polarimetric measurements, and eventually reveal more about the interplay of turbulence and the magnetic field lines. In this work we make 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 intensity emitted and polarization degree for the simulated models. We were able to reproduce the decay of the polarization degree at denser regions without any assumption regarding the properties of the dusty component. The anti-correlation arises from the simple cancellation 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 function, the power spectrum, and the structure function of the polarization angles. This statistical analysis revealed strong differences 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. (AU) | |