Mapping the surface of pulsating magnetic stars with Zeeman-Doppler imaging

Zeeman-Doppler Imaging (ZDI) is a technique that inverts a series of spectropolarimetric data allowing the reconstruction of the magnetic geometry and field strength of a star. It has been proven to be a powerful tool in understanding the complexity and configuration of stellar magnetic fields. Previously, it has been performed on the assumption that both the surface brightness and line profiles vary only with rotation. These are not valid assumptions for pulsating stars and can lead to errors in the magnetic field strength and geometry. I present the application to modelled pulsating stars of the first code able to correctly map the surface of magnetic pulsators, and contrast it to results that would be achieved by standard ZDI. By modelling the pulsations which could be observed by space photometry missions like TESS, we can include their additional effects in new time-dependent surface brightness maps and synthetic line profiles to fit spectropolarimetric observations. This modification of the open source ZDI code of Folsom et al. (2018) will lead to improved accuracy in stellar and magnetic properties, allowing us to perform a rigorous analysis of magneto-asteroseismic data, an essential step in the magneto-asteroseismic modelling of the internal structure of stars.