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A multi-model approach to X-ray pulsars - Connecting spectral and timing models to pin down the intrinsic emission characteristics of magnetized, accreting neutron stars

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Figure

Figure 1. Illustration of the formation of the intrinsic radiationat the base of the accretion column using a hybrid modelapproach for the continuum generation and for CRSF formationin a photosphere around the optically thick core
Figure 2. (Simplified) illustration of the effect ofmixing of radiation from both poles for a farobserver
Figure 3. Evolution of an example pulse profile over energy (grey lines: energy increasing from top to bottom).The energy-averaged pulse profile is shown as a black line for comparison (flux not to scale)
Figure 4. Example for a particularly strongvariability of the cyclotron line shapes with spinphase

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