Observational data on long-period oscillations in the angular velocity of pulsars are examined. The characteristic radii of the superfluid regions of pulsars are determined assuming that these oscillations are collective elastic oscillations of a superfluid vortex lattice (Tkachenko oscillations). These radii are compared with values obtained in various theoretical models of neutron stars which assume the existence of a superfluid quark “CFL”-core or a superfluid hyperon core. This method can be used to estimate the radii of pulsars.
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Translated from Astrofizika, Vol. 54, No. 1, pp. 131–137 (February 2011).
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Shahabasyan, K.M., Shahabasyan, M.K. Oscillations in the angular velocity of pulsars. Astrophysics 54, 111–116 (2011). https://doi.org/10.1007/s10511-011-9162-0
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DOI: https://doi.org/10.1007/s10511-011-9162-0