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Spectrum and pulse profile formation in strong field X ray pulsars

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Figure

Figure 1.1 Schematic showing the accretion geometry of X-ray pulsars (not to scale) relative to the neutron star rotation axis by poles
Table 2.1 Spectral parameters used for the galactic ridge component in fits to GX 1+4
Figure 2.1 The model geometry (only one column shown for clarity). The neutron star within zone value is 1 km
Figure 2.2  Monte-Carlo simulation results from single scattering of monoenergetic photons (To = 6.4 keV) in a plasma cloud with temperature Te
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