Abstract
THEORETICALLY, the structure of a rotating neutron star can support a variety of oscillations which may coexist with and couple to its surface rotation. Because it seems extremely probable that the pulsar period is kept by the rotating surface of a neutron star, the excitation of such modes would give small periodic modulations in observed pulsar frequencies. Most oscillatory modes have relatively high frequencies. But one does exist, unique to a rotating sphere of neutron superfluid, which has a period of about 4 months—close to the “wobble” reported for the period of the Crab pulsar1. The frequency of the oscillation mode of the rotating superfluid is insensitive to unknown parameters describing the stellar interior.
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RUDERMAN, M. Long Period Oscillations in Rotating Neutron Stars. Nature 225, 619–620 (1970). https://doi.org/10.1038/225619a0
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DOI: https://doi.org/10.1038/225619a0
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