Axisymmetric and stationary structures of magnetized barotropic stars with extremely strong magnetic fields deep inside
Axisymmetric and stationary structures of magnetized barotropic stars with extremely strong magnetic fields deep inside
复制标题
内部深处具有极强磁场的磁化正压星的轴对称和静止结构
DOI：
10.1111/j.1365-2966.2012.20614.x
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发表时间：
2012
影响因子：
4.8
通讯作者：
Y. Eriguchi
中科院分区：
文献类型：
--
作者：
K. Fujisawa;S. Yoshida;Y. Eriguchi
我们已经成功地获得了磁化的星星模型，这些模型在星星内部具有极强的磁场。在我们的公式中，磁通量函数的任意函数出现在电流密度的表达式中。通过适当地选择对应于环形电流密度分布的任意函数之一的函数形式，我们已经获得了具有高度局部化的中心部分和磁轴区域附近的磁场分布的配置。中心磁场的绝对值比表面区域强两个数量级。通过将我们的结果应用于磁星，内部磁极向场可以是1017 G，尽管磁星的表面磁场约为1015 G。对于白色矮星，当表面磁场为109 - 1010 G时，内部极向场可达1012 G.
We have succeeded in obtaining magnetized star models that have extremely strong magnetic fields in the interior of the star. In our formulation, arbitrary functions of the magnetic flux function appear in the expression for the current density. By appropriately choosing the functional form for one of the arbitrary functions that corresponds to the distribution of the toroidal current density, we have obtained configurations with magnetic field distributions that are highly localized within the central part and near the magnetic axis region. The absolute values of the central magnetic fields are stronger than those of the surface region by two orders of magnitude. By applying our results to magnetars, the internal magnetic poloidal fields could be 1017 G, although the surface magnetic fields are about 1015 G in the case of magnetars. For white dwarfs, the internal magnetic poloidal fields could be 1012 G, when the surface magnetic fields are 109–1010 G .