Abstract
Magneto‐elastic oscillations of neutron stars are believed to explain the observed quasi‐periodic oscillations (QPOs) in the decaying tail of the giant flares of highly magnetized neutron stars (magnetars). Strong efforts by theoretical modeling from different groups have increased our understanding of this phenomenon significantly. Here we discuss some constraints on the matter in neutron stars that arise if the interpretation of the observations in terms of superfluid magneto‐elastic oscillations is correct. To explain the observed modulation of the light curve of the giant flare, we describe a model that allows the QPOs to couple to the stellar exterior through the magnetic field. In this magnetosphere, the shaking magnetic field induces currents that provide scattering targets for resonant cyclotron scattering of photons, which is calculated with a Monte Carlo approach and coupled to a code that calculates the momentum distribution of the charge carriers as a one‐dimensional accelerator problem. We show first results of a simplified, but self‐consistent momentum distribution, that is a water‐bag distribution, and the corresponding spectra.
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