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Scattering of the forward‐shock synchrotron emission by a relativistic outflow located behind the leading blast wave may produce an X‐ray emission brighter than that coming directly from the forward shock and may explain four features displayed by  Swift  X‐ray afterglows: flares, plateaus (slow decays), chromatic light‐curve breaks and fast post‐plateau decays. For a cold scattering outflow, the reflected flux overshines the primary one if the scattering outflow is nearly baryon‐free and highly relativistic. These two requirements can be relaxed if the scattering outflow is energized by weak internal shocks, so that the incident forward‐shock photons are also inverse‐Compton scattered, in addition to bulk scattering. Sweeping‐up of the photons left behind by the forward shock naturally yields short X‐ray flares. Owing to the boost in photon energy produced by bulk scattering, the reflected emission is more likely to overshine that coming directly from the forward shock at higher photon energies, yielding light‐curve plateaus and breaks that appear only in the X‐ray. The brightness, shape and decay of the X‐ray light‐curve plateau depend on the radial distribution of the scatterer's Lorentz factor and mass flux. Chromatic X‐ray light‐curve breaks and sharp post‐plateau decays cannot be accommodated by the direct forward‐shock emission and argue in favour of the scattering‐outflow model proposed here. On the other hand, the X‐ray afterglows without plateaus, those with achromatic breaks and those with very long lived power‐law decays are more naturally accommodated by the standard forward‐shock model. Thus, the diversity of X‐ray light curves arises from the interplay of the scattered and direct forward‐shock emissions.

X‐ray flares, plateaus and chromatic breaks of GRB afterglows from up‐scattered forward‐shock emission