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Paper: X-ray Spectrum and Pulsations of the Vela Pulsar
Volume: 271, Neutron Stars in Supernova Remnants
Page: 353
Authors: Sanwal, D.; Pavlov, G. G.; Kargaltsev, O. Y.; Garmire, G. P.; Zavlin, V. E.; Burwitz, V.; Manchester, R. N.; Dodson, R.
Abstract: We report the results of spectral and timing analysis of observations of the Vela pulsar with the Chandra X-ray Observatory. The spectrum shows no statistically significant spectral lines in the observed 0.25-8.0 keV band. It consists of two distinct continuum components. The softer component can be modeled as either a magnetic hydrogen atmosphere spectrum with kTeff,infty = 59+-3 eV, Rinfty = 15.5+-1.5 km, or a standard blackbody with kTinfty = 129+-4 eV, Rinfty = 2.1+-0.2 km (the radii are for a distance of 250 pc). The harder component, modeled as a power-law spectrum, gives photon indices depending on the model adopted for the soft component: Gamma = 1.5+-0.3 for the magnetic atmosphere soft component, and Gamma = 2.7+-0.4 for the blackbody soft component. Timing analysis shows three peaks in the pulse profile, separated by about 0.3 in phase. Energy-resolved timing provides evidence for pulse profile variation with energy. The higher energy (E > 1.8 keV) profile shows significantly higher pulsed fraction.
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