2007ApJ...669..570M

The ∼10⁴ yr old Vela Pulsar represents the bridge between the young Crab-like and the middle-aged rotation-powered pulsars. Its multiwavelength behavior is due to the superposition of different spectral components. We take advantage of the unprecedented harvest of photons collected by XMM-Newton to assess the Vela Pulsar spectral shape and to study the pulsar spectrum as a function of its rotational phase. As for the middle-aged pulsars Geminga, PSR B0656+14, and PSR B1055-52 (the ``Three Musketeers''), the phase-integrated spectrum of Vela is well described by a three-component model, consisting of two blackbodies (T_bb=[1.06±0.03]x10⁶ K, R_bb=5.1^+0.4_–0.3km, T_BB=2.16^+0.06_–0.07x10⁶ K, R_BB=0.73^+0.09_–0.07km) plus a power law (γ=2.2^+0.4_–0.3). The relative contributions of the three components are seen to vary as a function of the pulsar rotational phase. The two blackbodies have a shallow ∼7%-9% modulation. The cooler blackbody, possibly related to the bulk of the neutron star surface, has a complex modulation, with two peaks per period, separated by ∼0.35 in phase, the radio pulse occurring exactly in between. The hotter blackbody, possibly originating from a hot polar region, has a nearly sinusoidal modulation, with a single, broad maximum aligned with the second peak of the cooler blackbody, trailing the radio pulse by ∼0.15 in phase. The nonthermal component, magnetospheric in origin, is present only during 20% of the pulsar phase and appears to be opposite to the radio pulse. XMM-Newton phase-resolved spectroscopy unveils the link between the thermally emitting surface of the neutron star and its charge-filled magnetosphere, probing emission geometry as a function of the pulsar rotation. This is a fundamental piece of information for future three-dimensional modeling of the pulsar magnetosphere.