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We present analysis of 100 ks contiguous XMM-Newton data of the prototypicalwind accretor Vela X-1. The observation covered eclipse egress between orbitalphases 0.134 and 0.265, during which a giant flare took place, enabling us tostudy the spectral properties both outside and during the flare. This giantflare with a peak luminosity of $3.92^{+0.42}_{-0.09} \times 10^{37}$ ergs$^{-1}$ allows estimates of the physical parameters of the accreted structurewith a mass of $\sim$ $10^{21}$ g.  We have been able to model several contributions to the observed spectrumwith a phenomenological model formed by three absorbed power laws plus threeemission lines. After analysing the variations with orbital phase of the columndensity of each component, as well as those in the Fe and Ni fluorescencelines, we provide a physical interpretation for each spectral component.Meanwhile, the first two components are two aspects of the principal accretioncomponent from the surface of the neutron star, and the third component seemsto be the \textit{X-ray light echo} formed in the stellar wind of thecompanion.

The accretion environment in Vela X-1 during a flaring period using XMM-Newton