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强磁化中子星的平衡态研究

Equilibrium Configurations of Strongly Magnetized Neutron Stars with Realistic Equations of State

Kenta Kiuchi, Kei Kotake

备注：
submitted to MNRAS
发表信息：
Mon.Not.Roy.Astron.Soc.385:1327-1347,2008
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摘要：

我们用四种SLy（Douchin et al.）的实际状态方程（EOSs）研究了磁化旋转星的平衡序列，FPS（Pandharipande等人），Shen（Shen等人），和LS（Lattimer & Swesty）。采用Tomimura-Eriguchi方案构造平衡构型。我们在牛顿引力的框架下研究了该序列的基本物理性质。此外，我们新考虑了广义相对论效应对磁化旋转组态的影响。通过这些计算，我们发现牛顿磁化星的性质，例如，磁场的结构，高度依赖于EOS。与SLy和FPS EOS相比，Shen和LS EOS的环形磁场更靠近表面。极向场也受到环形结构的影响。注意到的EOSs的刚度，我们详细分析了这种趋势。在广义相对论性恒星中，我们发现，由于EOSs的差异变得很小，因为所有使用的EOSs变得足够大的最大密度，通常大于$10^{15}\rm{g} \rm{cm}^{-3}$刚性。轴比为$q\sim 0.7$的磁化星的最大重子质量比球形星的最大重子质量增加约20倍。此外，我们计算在有限温度下的平衡序列，这应该作为一个初始条件的流体动力学研究的新生磁星。我们的研究结果表明，我们可以从观测磁星的质量中获得有关恒星的信息。

英文摘要：

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 $10^{15}\rm{g} \rm{cm}^{-3}$. 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.

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