  The observed large rates of spinning down after glitches in some radio
pulsars have been previously explained in terms of a long-term spin-up behavior
of a superfluid part of the crust of neutron stars. We argue that the suggested
mechanism is not viable; being inconsistent with the basic requirements for a
superfluid spin-up, in addition to its quantitative disagreement with the data.
Hence, the observed post-glitch relaxations may not be interpreted due only to
the effects of the stellar crust.
