is $\approx 62^\circ$.

(80mm,80mm)[figure3.eps]{}

Discussion and Conclusion
=========================

(80mm,80mm)[figure4.eps]{} \[fig:dis01\]

Let us discuss the structure of the global magnetosphere on the basis of our results. In figure \[fig:dis01\], we summarize electromagnetic properties of each magnetospheric region. There is a possibility that multiple acceleration regions exist in a different way from the traditional picture because of the current-neutral zone.

First, we discuss Region A and Region B. In PC and SG models, the side boundary condition is that $\Phi=0$ along the last open field lines. In our simulation, the side boundary of the polar flows correspond to the rim of Region B. Therefore, the surface of Region B plays the role of the side boundary of PC and SG models, instead of the traditional dead zone. The boundary condition on the neutron star surface depends on conditions such as the surface temperature, the surface magnetic field strength, and the atomic number of matter in the surface layer. In the case of most pulsars, one may assume $E_{||}=0$ and $\Phi=0$ for the boundary conditions on the stellar surface. As described in the previous section, the strong $E_{||}$ just above the magnetic poles (figure \[fig:dis01\]) includes the artificial effects, which are caused by 