the profiles of the plasma $\beta$ on the $\theta = \pi / 2$ plane, i.e. on the equatorial plane. Here, the plasma $\beta$ is defined as follows: $$\begin{aligned}
 \beta = 8 \pi p / |\Vec{H}|^2 .\end{aligned}$$ This quantity denotes the contribution of the gas pressure effect compared with the magnetic pressure effect. Fig. \[fig:beta\] shows profiles of $\beta$ for models with $m = -2.0, 0.0, 1.0$. As seen from Fig.\[fig:beta\], the profiles of $\beta$ are very similar to each other near the stellar surface regions. For the region around $\hat{r} \sim 0.6$, however, the value of $\beta$ for the $m=-2.0$ model is larger than those for the $m=0$ and $m=1.0$ models. Since these models have almost the same mass density distributions, this difference means a difference of magnetic pressure distribution. In this region the magnetic field of the $m=-2.0$ configuration is weaker and thus the $\beta$ becomes larger. However, [*it should be noted that*]{} these contours for the model with $m=-2.0$ are rather confined to the very narrow region near the central part. In other words, the gradient of the magnetic field distribution for the model with $m = -2$ is much steeper than the gradient of the gas pressure 