Abstract We present a spectropolarimetric study of the nearby M4.5V exoplanet host star YZ Cet, based on near-infrared observations obtained with the Spectropolarimètre Infrarouge at the Canada-France-Hawaii Telescope. We detect striking changes in the large-scale magnetic field strength and geometry over the course of just a few stellar rotations, a level of short-term global magnetic field evolution rarely reported in M dwarfs. We modeled the temporal variation of the longitudinal magnetic field using the Gaussian process regression, which allowed us to robustly determine the stellar rotation period and quantify the evolution timescale of the magnetic field. Independent Zeeman Doppler imaging reconstructions of the two epochs confirm a significant reconfiguration of the star’s global magnetic strength and topology. The detection of a weaker complex axisymmetric magnetic field (mean ∣ B ∣ ∼ 201 G), which changes into a stronger nonaxisymmetric dipole-dominated field (Mean ∣ B ∣ ∼ 276 G) over a few rotation cycles, is in contrast to results from similar fully convective M dwarf stars. YZ Cet is known to exhibit polarized radio bursts potentially driven by auroral radio emission from star–planet interaction (SPI). By combining our magnetic maps with recent radio observations, we refine the constraints on the magnetic field strength of the innermost planet, YZ Cet b. These results underscore the importance of monitoring stellar magnetic variability to interpret multiwavelength SPI signatures and to characterize the magnetospheres of potentially habitable exoplanets.
Biswas et al. (2026) studied this question.