2025MNRAS.539.3077P

SiO masers from AGB stars exhibit variability in intensity and polarization during a pulsation period. This variability is explained by radiative transfer and magnetic properties of the molecule. To investigate this phenomenon, a 3D maser simulation is employed to study the SiO masers based on Zeeman splitting. We demonstrate that the magnetic field direction affects maser polarization within small tubular domains with isotropic pumping, and yields results that are similar to those obtained from 1D modelling. This work also studies larger clouds with different shapes. We use finite-element domains with internal node distributions to represent the maser-supporting clouds. We calculate solutions for the population inversions in all transitions and at every node. These solutions show that saturation begins near the middle of a domain, moving towards the edges and particularly the ends of long axes, as saturation progresses, influencing polarization. When the observer's view of the domain changes, the plane of linear polarization responds to the projected shape and the projected magnetic field axis. The angle between the observer's line of sight and the magnetic field may cause jumps in the plane of polarization. Therefore, we can conclude that polarization is influenced by both the cloud's major axis orientation and magnetic field direction. We have investigated the possibility of explaining observed polarization plane rotations, apparently within a single cloud, by the mechanism of line-of-sight overlap of two magnetized maser clouds.