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A rotating fluid star, endowed with a magnetic field, can undergo a form ofprecessional motion: a sum of rigid-body free precession and a non-rigidresponse. On secular timescales this motion is dissipated by bulk and shearviscous processes in the stellar interior and magnetospheric braking in theexterior, changing the inclination angle between the rotation and magneticaxes. Using our recent solutions for the non-rigid precessional dynamics, andviscous dissipation integrals derived in this paper, we make the onlyself-consistent calculation to date of these dissipation rates. We present thefirst results for the full coupled evolution of spindown and inclination anglefor a model of a late-stage proto-neutron star with a strong toroidal magneticfield, allowing for both electromagnetic torques and internal dissipation whenevolving the inclination angle. We explore this coupled evolution for a rangeof initial inclination angles, rotation rates and magnetic field strengths. Forfixed initial inclination angle, our results indicate that the neutron-starpopulation naturally evolves into two classes: near-aligned and near-orthogonalrotators -- with typical pulsars falling into the latter category. Millisecondmagnetars can evolve into the near-aligned rotators which mature magnetarsappear to be, but only for small initial inclination angle and internaltoroidal fields stronger than roughly $5\times 10^{15}$ G. Once any model hasevolved to either an aligned or orthogonal state, there appears to be nofurther evolution away from this state at later times.

Neutron-star spindown and magnetic inclination-angle evolution