-0.5   1.3E-4               1.02E+1                     9.972E-1             2.21E-5        3.33E-1    5.07E-2       1.41E-4       8.35E-7    2.788E-6                 
   0.0    8.8E-5               7.17E+0                     9.968E-1             1.99E-5        3.33E-1    5.07E-2       5.25E-3       8.31E-7    2.789E-6                 
   0.5    7.0E-5               5.69E+0                     9.963E-1             1.83E-5        3.33E-1    5.07E-2       1.92E-1       8.23E-7    2.789E-6                 
   1.0    6.1E-5               4.78E+0                     9.959E-1             1.70E-5        3.33E-1    5.07E-2       6.90E+0       8.11E-7    2.789E-6                 

![image](img/fig2_ul.eps) ![image](img/fig2_ur.eps)

![image](img/fig2_ml.eps) ![image](img/fig2_mr.eps)

![image](img/fig2_bl.eps) ![image](img/fig2_br.eps)

![image](img/fig3.eps)

![image](img/fig4_l.eps) ![image](img/fig4_c.eps) ![image](img/fig4_r.eps)

![image](img/fig5_l.eps) ![image](img/fig5_c.eps) ![image](img/fig5_r.eps)

We show the results for the distributions of the magnetic fields for different values of $m$. In particular, in order to examine the effect of magnetic fields alone, we consider configurations without rotation. The effect of stellar rotation is discussed in Sec. \[Sec:rotation\]. Thus we set $\hat{\Omega}_0 = 0$ and compute $N=1$ polytropic equilibrium models with different values of $ m$ and appropriate values of $q$ so that the surface magnetic field becomes roughly $H_{sur} = 10^{15}$ G when $\rho_c = 1.0 \times 10^{15} \mathrm{g cm^{-3}}$ and mass $M = 1.4 M_\odot$. By setting $N=1$ and an appropriate choice of polytropic constant $K$ of $p=K\rho^{2}$, we obtain models with $M=1.4M_\odot$. It should be noted that these models have the typical mass and radius for neutron stars. We choose $N=1$ as a simple approximation of neutron stars here. We searched and found the value of $q$ by calculating 