Poloidal magnetic fields in superconducting neutron stars
Poloidal magnetic fields in superconducting neutron stars
复制标题
超导中子星的极向磁场
DOI：
--
复制
发表时间：
2012
期刊：
影响因子：
--
通讯作者：
I. Wasserman
中科院分区：
文献类型：
--
作者：
K. Henriksson;I. Wasserman
本文发展了一种计算轴对称中子星星内部磁场的形式，该中子星具有被正常导体包围的强II型超导体核。形式主义充分考虑了正压状态方程的流体静力平衡所施加的约束。我们专注于纯极向磁场，并开发了“最偶极的情况下”，我们发现，表面场强度是$\simeq H_B\xBB_B/3\simeq 3\times 10^{12}$ G，其中$H_B$是在核心的外边缘的磁场和$\xBB_B R$是正常壳的厚度。这个值只取决于核物质的状态方程。我们还发现该星星的四极失真为$\sim 10^{-9}$。
We develop the formalism for computing the magnetic field within an axisymmetric neutron star with a strong Type II superconductor core surrounded by a normal conductor. The formalism takes full account of the constraints imposed by hydrostatic equilibrium with a barotropic equation of state. We specialize to purely poloidal magnetic fields and develop the "most dipolar case" for which we find that the surface field strength is $\simeq H_b\epsilon_b/3\simeq 3\times 10^{12}$ G, where $H_b$ is the magnetic field at the outer edge of the core and $\epsilon_b R$ is the thickness of the normal shell. This value only depends on the equation of state of nuclear matter. We also find that the quadrupolar distortion of the star is $\sim 10^{-9}$.