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tokens: field, S , exists near the pole. This result is due to spatial symmetry. Figure 4 shows the time-averaged toroidal flux S in . The toroidal magnetic field S decreases gradually by the radius from the star. The maximum value of S falls inside the light cylinder radius. The maximum value does not match the radius of the light cylinder. The concentrated poloidal current area is the light cylinder interior. Figure 4. Time-averaged toroidal magnetic flux function S for the center of the star. . The toroidal magnetic field, S , increases due to large electrical conductivity . In our model, the value increases with the increase of r Equation ( 49 ). The toroidal magnetic field increase proportionally to electrical conductivity. Figure 3 (c) shows the electromagnetic field for , five times bigger than the case. In addition, this field area spreads out. This is in contrast to the poloidal magnetic field G , which is not changed by the electrical conductivity. 4.1.3. Electrostatic Potential Φ Figure 5 (a) shows the electrostatic potential contour of . From to 0.08, contours are equally spaced for each 0.01. In the numerical calculation, the electrostatic potential on the star’s surface does not change with time because of the boundary conditions Equation ( 36 ). Blue lines in Figure 5 (a) spread out from the surface boundary and extend in the radial direction. Blue lines are connected vertically toward the equatorial plane because the field’s boundary condition has only an R component in this plane. Figure 5 (b) shows the electrostatic potential of the spatial region from Z = 0 to 30. Here, the contour line is drawn in increments of 0.005 from . Figure 5. Electrical potential Φ for . The red line is the light cylinder radius R = 5. The black line is the equal value of the poloidal-magnetic flux function G . The black dotted line shows a dipole-magnetic flux equal to the value of the function. The bottom panels show zoomed-out views. The densities of the equipotential lines are proportional to the strength of the electric field, which is strong on the star surface and decreases as one goes radially outward. No electric field dominant () area exist in . The magnetic field in the obtained results is always stronger than the electric field. Figure 5 (c) is the drawn contours of the electrostatic potential cases. Electrical conductivity increases along with the electrostatic potential of the equatorial plane. However, the difference of electrostatic potential of the equatorial plane between the and is about 10%. When the electrical conductivity is different from this case, the overall structure of the solution remains similar. For example, electrical conductivity is increased in a toroidal magnetic field, but little shape change was observed about the potential. 4.1.4. Poloidal Current j<sub>p</sub> Current density is divided into poloidal and toroidal components. The poloidal component of current density j p consists of j r and : Figure 6 (a) plots