In case of CSC, the field creation and evolution may also be influenced significantly if there exist fast dynamos with magnetic Reynolds number ${\cal R}_{\rm m} \rightarrow \infty$ in PSSs.

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The density model $\rho_0(r_0) = \rho_{01} {\rm e}^{-\alpha_1 r_0}$ with $\rho_{01}=2~10^{10}$ g cm^-3, $\alpha_1=5.4~10^{-8}$ cm^-1, based on which we will calculate the nature of differential rotation of PSSs (or PNSs), represents well the initial core model of Bruenn (1985, Fig. 1, there $R_0\sim 10^8$ cm, ${\cal M}(10^8)\sim 1.4~M_\odot$ , $\rho_0(0) = 2~10^{10}$ g cm^-3, and $\rho_0(10^8) = 8~10^7$ g cm^-3). We thus think that the computation according to this simplified density model can give the correct order of magnitude result for the actual collapsed rotating core.

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...1998)

The recent observation of spin-kick alignment of Crab and Vela pulsars supports this suggestion.

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