field is a strong reminiscence of magnetically driven outflows model [@Huarte2012] and is also supported by the possible presence of an helical field, inferred by the distribution of the polarization vectors (i.e. PA variation) in the 230 GHz polarization map (Fig.\[Tower\]).\
Now that we have established the presence of a multi-scale magnetic field in OH 231.8+4.2 we can postulate that it might have a dynamical role in the shaping of the nebula.\
The polarization vectors seen at millimeter and sub-mm wavelengths could indicate the presence of frozen-in toroidal magnetic field lines which would have subsequently been dragged along with the outflows, but they could also trace the remnant of a dynamo-generated magnetic field which has evolved in time. In the later scheme the field is amplified in the rotating disk/torus or within the binary system. The smaller the disk or the closer the binary separation, the higher the magnetic field intensity, and therefore we would expect a magnetic launching mechanism. MHD launching is very likely the only process that would reproduce the kinetic energies observed in such evolved nebulae [@Garcia2020]. Hence, [@Huarte2012] (and references therein) discussed two magnetic models, which could account for the observed magnetic structure in OH 231.8+4.2: 