We investigate equilibrium sequences of magnetized rotating stars with four kinds of realistic equations of state ( EOSs ) of SLy ( Douchin et al .
) , FPS ( Pandharipande et al .
) , Shen ( Shen et al .
) , and LS ( Lattimer & Swesty ) .
Employing the Tomimura-Eriguchi scheme to construct the equilibrium configurations .
we study the basic physical properties of the sequences in the framework of Newton gravity .
In addition we newly take into account a general relativistic effect to the magnetized rotating configurations .
With these computations , we find that the properties of the Newtonian magnetized stars , e.g. , structure of magnetic field , highly depends on the EOSs .
The toroidal magnetic fields concentrate rather near the surface for Shen and LS EOSs than those for SLy and FPS EOSs .
The poloidal fields are also affected by the toroidal configurations .
Paying attention to the stiffness of the EOSs , we analyze this tendency in detail .
In the general relativistic stars , we find that the difference due to the EOSs becomes small because all the employed EOSs become sufficiently stiff for the large maximum density , typically greater than 10 ^ { 15 } g~ { } cm ^ { -3 } .
The maximum baryon mass of the magnetized stars with axis ratio q \sim 0.7 increases about up to twenty percents for that of spherical stars .
We furthermore compute equilibrium sequences at finite temperature , which should serve as an initial condition for the hydrodynamic study of newly-born magnetars .
Our results suggest that we may obtain information about the EOSs from the observation of the masses of magnetars .