赤道非对称磁化超新星的数值模拟：磁星的形成及其反冲
Numerical Simulations of Equatorially-Asymmetric Magnetized Supernovae: Formation of Magnetars and Their Kicks
摘要：
对磁旋转核塌缩超新星进行了一系列数值模拟。假设最初的强磁场与快速的差分旋转偏北的偶极状配置。我们的研究目的是探讨偏移磁场对磁星反冲和超新星动力学的影响。请注意，我们研究的是一个区域，其中坍缩后形成的原中子星具有接近“磁星”的大磁场强度，“磁星”是一种高度磁化的缓慢旋转的中子星。因此，赤道非对称爆炸发生的双极射流的形成。由此产生的磁星反冲速度为$\sim 300-1000$ km s $^{-1}$。我们发现，加速主要是由于磁压的作用，而稍弱的磁张力则相反，这是由于北半球较强的磁场造成的。注意到磁星自行的观测是非常稀缺的，我们的结果提供了一个预测未来的观测。也就是说，磁星可能像普通的中子星一样，具有几百公里/秒的大反冲速度$^{-1}$，在极端情况下，它们的反冲速度可以达到1000公里/秒的$^{-1}$。
英文摘要：
A series of numerical simulations on magnetorotational core-collapse supernovae are carried out. Dipole-like configurations which are offset northward are assumed for the initially strong magnetic fields together with rapid differential rotations. Aims of our study are to investigate effects of the offset magnetic field on magnetar kicks and on supernova dynamics. Note that we study a regime where the proto-neutron star formed after collapse has a large magnetic field strength approaching that of a ``magnetar'', a highly magnetized slowly rotating neutron star. As a result, equatorially-asymmetric explosions occur with a formation of the bipolar jets. Resultant magnetar's kick velocities are $\sim 300-1000$ km s$^{-1}$. We find that the acceleration is mainly due to the magnetic pressure while the somewhat weaker magnetic tension works toward the opposite direction, which is due to stronger magnetic field in the northern hemisphere. Noted that observations of magnetar's proper motions are very scarce, our results supply a prediction for future observations. Namely, magnetars possibly have large kick velocities, several hundred km s$^{-1}$, as ordinary neutron stars do, and in an extreme case they could have those up to 1000 km s$^{-1}$.
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