Rapid quasi-periodic reconfiguration of the accretion column in pulsar 1A 0535+262

Accretion onto strongly magnetised neutron stars is commonly interpreted using quasi-steady models, in which the accretion-column structure adjusts smoothly to the mass inflow rate. The cyclotron line in the X-ray spectrum, whose centroid energy traces the magnetic field strength and thus the height of the line-forming region, provides a key diagnostic of this structure. Whether this simple quasi-steady description remains valid on short dynamical timescales has remained uncertain. Here we show that, during a giant outburst of the X-ray pulsar 1A 0535+262, quasi-periodic hard X-ray flux variations are accompanied by synchronised oscillations of the cyclotron line energy, with amplitudes exceeding those expected from simple accretion-rate fluctuations. The anti-correlation between cyclotron energy and apparent flux provides direct spectral-timing evidence for rapid changes in the line-forming region, which we interpret as geometric reconfiguration of the accretion column. The variability emerges in the luminosity regime where radiation pressure becomes dynamically important. These results reveal limitations of a simple quasi-steady interpretation for this source and suggest that radiation-supported columns can enter intrinsically dynamical states in high-luminosity accreting pulsars. At neutron-star poles, extreme magnetic fields can pile falling gas from its companion into luminous columns that power brightest X-ray lighthouses in Universe. Here, the authors show that in 1A 0535+262 this column rhythmically changes size as internal radiation pressure begins to dominate.