Rotating, magnetized neutron stars can support a rich variety of oscillation modes. The periods of the modes are estimated and compared with periodicities found in the pulsars. The millisecond time scale quasi-periodic micropulsations observed in PSR 2016+28 and PSR 1133+16 can be identified as nonradial l = 0 or 1 p-mode oscillations, if mode-beating or internal noise broadening can account for the apparent rapid variability of amplitude and frequency. Torsional oscillations of the neutron star crusts have periods in the range of the pulsar subpulses; and rotational splitting of modes with l = 2, 3, or 4 can account qualitatively for subpulse drift. Long-period Alfvén modes, as well as Tkachenko oscillations, should be excited by pulsar glitches, and postglitch data may contain direct evidence of these modes.
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H. M. van Horn (1980) studied this question.