X-ray Spectrum and Pulsations of the Vela Pulsar

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dc.creatorSanwal, D.
dc.creatorPavlov, G. G.
dc.creatorKargaltsev, O. Y.
dc.creatorGarmire, G. P.
dc.creatorZavlin, V. E.
dc.creatorBurwitz, V.
dc.creatorManchester, R. N.
dc.creatorDodson, R.
dc.date2001-12-06
dc.date2001-12-12
dc.date.accessioned2026-07-07T02:01:44Z
dc.date.available2026-07-07T02:01:44Z
dc.descriptionWe report the results of the 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 kT = 59 +- 3 eV, R = 15.5 +- 1.5 km, or a standard blackbody with kT = 129 +- 4 eV, R = 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.
dc.description4 pages, 2 figures, To appear in "Neutron Stars in Supernova Remnants" (ASP Conference Proceedings), eds P. O. Slane and B. M. Gaensler Corrected TYPOS
dc.identifierhttps://arxiv.org/abs/astro-ph/0112164
dc.identifierhttp://arxiv.org/abs/astro-ph/0112164
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3858
dc.subjectAstrophysics
dc.titleX-ray Spectrum and Pulsations of the Vela Pulsar
dc.typetext

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