to obtain stationary configurations of the magnetized stars.

Concerning the evolution of the stellar magnetic fields, since it has been very difficult to pursue evolutionary computations of the global magnetic fields for both interiors and exteriors of stars, few results have been obtained. Recently, however, Braithwaite and his collaborators have succeeded in following the evolution of global stellar magnetic fields (@Braithwaite_Spruit_2004; @Braithwaite_Nordlund_2006; @Braithwaite_Spruit_2006; @Braithwaite_2006; @Braithwaite_2007; @Braithwaite_2008; @Braithwaite_2009; @Duez_Braithwaite_Mathis_2010). They found that the twisted-torus configurations of the magnetic fields inside stars seem to be stable across the dynamical timescale.

On the other hand, to investigate possible structures of the interior and exterior magnetic fields by imposing stationarity is a different theoretical approach. Concerning this problem, many attempts have been made but it has also been difficult to obtain stellar structures with both [*poloidal*]{} and [*toroidal*]{} non force-free magnetic fields self-consistently, not only in the Newtonian gravity but also in general relativity (see e.g. @Chandrasekhar_Fermi_1953; @Ferraro_1954; @Chandrasekhar_1956; @Chandrasekhar_Prendergast_1956; @Prendergast_1956; @Woltjer_1959a; @Woltjer_1959b; @Woltjer_1960; @Wentzel_1961; @Ostriker_Hartwick_1968; @Miketinac_1973; @Miketinac_1975; @Bocquet_et_al_1995; @Ioka_Sasaki_2004; @Kiuchi_Yoshida_2008; @Haskell_Samuelsson_Glampedakis_2008 ; @Duez_Mathis_2010). It is only recently that axisymmetric and stationary barotropic stellar structures have been successfully solved for configurations with both [*poloidal*]{} and [*toroidal*]{} magnetic components (@Tomimura_Eriguchi_2005; @Yoshida_Eriguchi_2006; @Yoshida_Yoshida_Eriguchi_2006; @Lander_Jones_2009; @Otani_Takahashi_Eriguchi_2009) in 