论文标题
原始中子星的一般相对论平均磁场模型
General Relativistic Mean-field Dynamo Model for Proto-neutron Stars
论文作者
论文摘要
尤其是中子星，尤其是磁铁，众所周知可以容纳宇宙中最强的磁场。这些强领域的起源是一个争议的问题。在这项初步工作中，通过数值模拟，我们首次在非理想的一般相对论磁性水力动力学（GRMHD）方向上研究，这是由于均衡，未解决的湍流而导致的均值磁场作用而引起的磁场的生长。发电机工艺与（原始恒星的差异旋转结合在一起）能够产生任何初始磁性种子场的指数生长，直到解释观测值所需的值。通过改变发电机系数，我们获得了不同的增长率。我们发现生长速率对发电机强度的准线性依赖性。此外，发生指数增长的时间间隔，增长率似乎还取决于磁场的初始配置。
Neutron stars, and magnetars in particular, are known to host the strongest magnetic fields in the Universe. The origin of these strong fields is a matter of controversy. In this preliminary work, via numerical simulations, we study, for the first time in non-ideal general relativistic magnetohydrodynamic (GRMHD) regime, the growth of the magnetic field due to the action of the mean-field dynamo due to sub-scale, unresolved turbulence. The dynamo process, combined with the differential rotation of the (proto-)star, is able to produce an exponential growth of any initial magnetic seed field up to the values required to explain the observations. By varying the dynamo coefficient we obtain different growth rates. We find a quasi-linear dependence of the growth rates on the intensity of the dynamo. Furthermore, the time interval in which exponential growth occurs and the growth rates also seems to depend on the initial configuration of the magnetic field.
