Magnetar quasi-periodic oscillations (QPO's) would be relatively easy to model, and thereby deduce properties of neutron stars, if all we needed to worry about is the crust. If only it were that easy.
There are two types of torsional modes in the neutron star: shear modes in the crust and alfven modes in the core. These two modes have similar frequencies, so we expect coupling between the modes. The timescale for energy exchange is much smaller than the duration of the QPO's, so we expect many exchanges to occur.
Therefore, we need a realistic model of the coupled crust and core to really understand magnetar QPO's.
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