2013MNRAS.430.1359T

We investigate the possibility that a magnetic field may be present in the star o-Ceti (hereafter Mira) and that the field plays a role in the star's mass loss. The model presented here is an application of an earlier derived theory that has been successfully applied for modelling the wind of a generic intermediate-mass asymptotic giant branch (AGB) star and that of the red supergiant star Betelgeuse, and is now extended to the low-mass end AGB stars, Mira. The modelling shows that it is possible to obtain a hybrid magnetohydrodynamic-dust-driven wind scenario for Mira, in which the magnetic field in the equatorial plane of the star is dynamically important for producing a stellar wind. The wind velocity and the temperatures obtained from the model appear consistent with observational findings elsewhere.