Present address: Department of Physics, University of Alberta, Edmonton AB, Canada T6G 2J1.

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Actually Sedrakian et al. (1999) have shown that even for partially pinned vortices the core and the crust would rotate at different angular velocities.

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... acceptable

Though such a short magnetic cycle has not been observed in neutron stars yet, the early observations of A-type stars ( $\alpha$ -variables), with kilogauss magnetic field strength, showed large amplitude, nearly symmetric magnetic reversals in periods ranging from 4 to 9 days, close to the periods of the stars (Babcock 1958). Several recent observations from the young rapidly rotating stars confirmed the existence of the solar-type magnetic cycle with $P_0/P_{\rm cyc}\simeq 10^{-4}$ (Brandenburg et al. 1998, Kitchatinov et al. 2000). Of course these stars presumably have active convection zone, for the case PSR B1828-11 with proposed period for the magnetic cycle, we have $P_0/P_{\rm cyc}\simeq 10^{-9}$ , which is smaller by 5 orders of magnitude relative to one obtained for the young rotating stars. This may agree with the fact that in neutron stars the convective fluid motions are hardly excited.

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... pulsar

It is interesting to note that according to the neutron star crustal tectonics scenario the magnetic fields in spinning down neutron stars move to achieve a right angle configuration relative to the star's spin axis (Ruderman 1991a,b). This is in agreement with our analysis for PSR B1828-11 as we found $\chi\geq 89^\circ$ .

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