Masses and radii of neutron stars are obtained in the presence of strong magnetic fields together with rotation. Mass-radius relations are calculated using eleven EoSs (GM1, TM1-a, TM1-b, TM2ωρ-a, TM2ωρ-b, NL3-a, NL3-b, NL3ωρ-a, NL3ωρ-b, DDME2-a and DDME2-b) in relativistic mean field (RMF) theory. Obtained masses are over and around twice the solar mass (M_⊙) for all EoSs in the presence of strong magnetic fields of 3 × 1018 G at the center. For NL3ωρ-a and NL3ωρ-b EoS, masses are more than M = 2.17 M_⊙(observed maximum mass : 2.14 M_⊙) even without magnetic fields. Rotational effects are found to be insignificant in any case, at least up to the Kepler frequency. Suitable EoSs are also selected concerning the constraint on the radius of a neutron star.

中文翻译：

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旋转时在强磁场中寻找中子星物质的最佳EoSs

中子星的质量和半径是在强磁场和自转共同作用下获得的。使用11个EoS（GM1，TM1-a，TM1-b，TM2ωρ-a，TM2ωρ-b，NL3-a，NL3-b，NL3ωρ-a，NL3ωρ-b，DDME2-a和DDME2- b）相对论平均场（RMF）理论。得到群众是上方和周围的太阳质量两次（中号_⊙在3×1018的G强磁场的中心处的存在所有EOSS）。对于NL3ωρ-a和NL3ωρ-B的EoS，群众超过中号= 2.17中号_⊙（观察到的最大的质量：2.14中号_⊙）甚至没有磁场。发现旋转效应在任何情况下都是微不足道的，至少直到开普勒频率为止。关于中子星半径的约束，还选择合适的EoS。