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We test a model recently proposed for the persistent hard X-ray emission frommagnetars. In the model, hard X-rays are produced by a deceleratingelectron-positron flow in the closed magnetosphere. The flow decelerates as itradiates its energy away via resonant scattering of soft X-rays, then itreaches the top of the magnetic loop and annihilates there. We test the modelagainst observations of three magnetars: 4U 0142+61, 1RXS J1708-4009, and 1E1841-045. We find that the model successfully fits the observed phase-resolvedspectra. We derive constraints on the angle between the rotational and magneticaxes of the neutron star, the object inclination to the line of sight, and thesize of the active twisted region filled with the plasma flow. Using the fit ofthe hard X-ray component of the magnetar spectrum, we revisit the remainingsoft X-ray component. We find that it can be explained by a modifiedtwo-temperature blackbody model. The hotter blackbody is consistent with a hotspot covering 1-10% of the neutron star surface. Such a hot spot is expected atthe base of the magnetospheric e+- outflow, as some particles created in thee+- discharge flow back and bombard the stellar surface.

Phase-resolved X-ray spectra of magnetars and the coronal outflow model