Abstract
The substantial differences between the X-ray pulse profiles seen during the «long-on» and the «short-on» stages in the 35 day cycle of Hercules X-1 are explained by a model that contains a tilted, twisted, precessing accretion disk, and an obliquely magnetized, nonprecessing neutron star which rapidly rotates about a fixed axis, perpendicular to the binary plane. The novel aspect of this model is a raised portion of the inner edge of the accretion disk that rotates synchronously with the neutron star. This additional component modulates the relative intensities of the main pulse and interpulse by attenuation of the emergent flux.
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