Abstract
Spinning down (or up) neutron star crusts can be stressed beyond their yield strengths by neutron superfluid vortex line pinning or magnetic field stresses. The spin history of a fast pulsar determines radio emission features which can be compared to those observed in millisecond pulsars. In young warm spinning-down neutron stars such as the Crab pulsar, crust flow should be largely plastic. Crusts of cooler stars such as the Vela pulsar may crack and give period glitches. In more slowly rotating (cool) neutron stars the glitches should be associated with intense bursts of gamma-rays.
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