We present J ^ { \prime } and K ^ { \prime } imaging linear polarimetric adaptive optics observations of NGC 1068 using MMT-Pol on the 6.5-m MMT .
These observations allow us to study the torus from a magnetohydrodynamical ( MHD ) framework .
In a 0 \aas@@fstack { \prime \prime } 5 ( 30 pc ) aperture at K ^ { \prime } , we find that polarisation arising from the passage of radiation from the inner edge of the torus through magnetically aligned dust grains in the clumps is the dominant polarisation mechanism , with an intrinsic polarisation of 7.0 % \pm 2.2 % .
This result yields a torus magnetic field strength in the range of 4 - 82 mG through paramagnetic alignment , and 139 ^ { +11 } _ { -20 } mG through the Chandrasekhar-Fermi method .
The measured position angle ( P.A . )
of polarisation at K ^ { \prime } is found to be similar to the P.A .
of the obscuring dusty component at few parsec scales using infrared interferometric techniques .
We show that the constant component of the magnetic field is responsible for the alignment of the dust grains , and aligned with the torus axis onto the plane of the sky .
Adopting this magnetic field configuration and the physical conditions of the clumps in the MHD outflow wind model , we estimate a mass outflow rate \leq 0.17 M _ { \odot } yr ^ { -1 } at 0.4 pc from the central engine for those clumps showing near-infrared dichroism .
The models used were able to create the torus in a timescale of \geq 10 ^ { 5 } yr with a rotational velocity of \leq 1228 km s ^ { -1 } at 0.4 pc .
We conclude that the evolution , morphology and kinematics of the torus in NGC 1068 can be explained within a MHD framework .