XMM Observations of Geminga, PSR B1055-52 and PSR B0656+14:. Phase Resolved Spectroscopy as a Tool to Investigate the X-γ Connection

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XMM-Newton observations of PSR B0656+14, PSR B1055-52 and Geminga have increased dramatically the statistics available for these three isolated neutron stars (INSs) so that it is now possible to perform phase resolved spectroscopy for all three objects. The phase-averaged spectrum of the three INSs is best described by a three component model including two blackbody curves, a cooler one, possibly originating from the bulk of the star surface, and a hotter one, coming from a smaller portion of the star surface (a "hot spot"), plus a power law. Dividing the pulsars' light curves in 10 identical phase intervals, we can study for the first time the evolution of the spectral shape as a function of the stars' rotation. Very dramatic (and highly significant) changes are clearly detected at specific phases. The relative contributions of the three components are seen to vary as a function of the pulsars' phase, as the stars' rotation bring into view different emitting regions. The hot spots, which have very different apparent dimensions (in spite of the similarity of the three neutron stars polar cap radii) are responsible for the bulk of the phase variation. Thus, the rotation of the neutron stars' surfaces can be directly seen for the first time.

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