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Accretion-powered X-ray pulsars offer a unique opportunity to study physicsunder extreme conditions. To fully exploit this potential, the interrelatedproblems of modelling radiative transport and the dynamical structure of theaccretion flow must, however, be solved. This task is challenging both from atheoretical and observational point of view and is further complicated by alack of direct correspondence between the properties of emission emerging fromthe neutron star and observed far away from it. In general, a mixture ofemission from both poles of the neutron star viewed from different angles isindeed observed at some or even all phases of the pulse cycle. It is essential,therefore, to reconstruct the contributions of each pole to the observed fluxin order to test and refine models describing the formation of the spectra andpulse profiles of X-ray pulsars. In this paper we propose a novel data-drivenapproach to address this problem using the pulse-to-pulse variability in theobserved flux, and demonstrate its application to RXTE observations of thebright persistent X-ray pulsar Cen X-3. We then discuss the comparison of ourresults with previous work attempting to solve the same problem and how theycan be qualitatively interpreted in the framework of a toy model describingemission from the poles of a neutron star.

Blind source separation for decomposing X-ray pulsar profiles. Introducing phase-correlated variability analysis (PCVA) with a case study of Cen X-3