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The observed long-term spin-down evolution of isolated radio pulsars cannotbe explained by the standard magnetic dipole radiation with a constant brakingtorque. However, how and why the torque varies still remains controversial,which is a major issue in understanding neutron stars. Many pulsars have beenobserved with significant long-term changes of their spin-down rates modulatedby quasi-periodic oscillations. Applying the phenomenological model of pulsartiming noise we developed recently to the observed precise pulsar timing dataof isolated neutron stars, here we show that the observed long-term evolutionsof their spin-down rates and quasi-periodic modulations can be explained byHall effects in their crusts. Therefore the evolution of their crustal magneticfields, rather than that in their cores, dominates the observed long termspin-down evolution of these young pulsars. Understanding of the nature ofpulsar timing noise not only reveals the interior physics of neutron stars, butalso allows physical modeling of pulsar spin-down and thus improves thesensitivity of gravitational wave detections with pulsars.

Interpreting the Spin-down Evolutions of Isolated Neutron Stars with Hall Effects