2025MNRAS.541.1913O

We present a long-term optical and X-ray photometric study of AN UMa, one of the prototypical polar-type cataclysmic variables, tracing more than 34 years of its accretion history. Observations from both ground-based and space-based facilities were analysed to investigate state transitions within the system. Throughout this period, significant changes in the light curve are observed, corresponding to different mass accretion states. From four years of The Transiting Exoplanet Survey Satellite (TESS) photometry, we derive a revised photometric period that agrees with the spectroscopic period to within 1.2$\sigma$. These optical observations further suggest switching between two accretion poles. During intervals of high accretion, dips in the X-ray light curve indicate that the primary accretion pole is obscured by an accretion stream elevated above the orbital plane, a feature also evident in the TESS light curves. Additionally, periodogram analysis reveals a periodicity of ∼437 d, which may be related to long-term accretion-state changes. Following a 16-yr high state, AN UMa entered two short-lived low states, lasting 180 and 123 d, during which it faded to a magnitude of 19.2, as recorded by the Zwicky Transient Facility (ZTF) and Asteroid Terrestrial-impact Last Alert System (ATLAS) surveys. Using the low-state brightness of the system and the distance provided by Gaia, we estimate that the system may have a white dwarf with an effective temperature of ∼15 000 K and a donor of spectral type M4.7. This work provides a useful reference for future studies of polars with variable accretion geometries and highlights the importance of long-term, multiwavelength monitoring in the study of magnetic cataclysmic variables.