论文标题
Magnetars的X射线亮度是否超过其旋转的亮度？
Do Magnetars' X-ray luminosities exceed their spin-down luminosities?
论文作者
论文摘要
磁铁的X射线照明量超过其旋转的亮度的普遍观点是基于以下假设：从磁铁中接收到的X射线的距离衰减的衰减遵守了反方规律。 The results presented here, of testing the hypothesis of independence of luminosities and distances of magnetars by means of the Efron-Petrosian statistic, do not uphold this assumption however: they imply that the observational data in the McGill Magnetar Catalog are consistent with the dependence S\propto D^{-3/2} of the flux densities S of these objects on their distances D at substantially higher levels of significance比与依赖关系s \ propto d^{-2}相比。这些结果与能量保护的要求并不兼容，因为Ardavan中描述的辐射过程（2021，Mnras，507，4530），通过该过程，中子星中的磁层中的超线移动的电流表被证明可以产生缓慢的衰减X射线脉冲，本质上是瞬时的。一旦纠正了它们的过度估计，X射线与旋转的亮度的比率始终低于1。磁体与其他旋转驱动的脉冲星的不同之处在于，相对于其自旋轴，沿特权的纬度方向观察到它：距离距离的距离越近，从电流板上的辐射聚焦，频率含量越高，并且观察到的辐射距离的衰减速率越高。因此，表征磁力发射的爆发是由于其自旋或磁轴的突然运动引起的。
The prevailing view that magnetars' X-ray luminosities exceed their spin-down luminosities is based on the assumption that the decay with distance of the flux of the X-rays received from magnetars obeys the inverse-square law. The results presented here, of testing the hypothesis of independence of luminosities and distances of magnetars by means of the Efron-Petrosian statistic, do not uphold this assumption however: they imply that the observational data in the McGill Magnetar Catalog are consistent with the dependence S\propto D^{-3/2} of the flux densities S of these objects on their distances D at substantially higher levels of significance than they are with the dependence S\propto D^{-2}. These results are not incompatible with the requirements of the conservation of energy because the radiation process described in Ardavan (2021, MNRAS, 507, 4530), by which the superluminally moving current sheet in the magnetosphere of a neutron star is shown to generate the slowly decaying X-ray pulses, is intrinsically transient. Once their over-estimation is rectified, the ratios of X-ray to spin-down luminosities of known magnetars turn out to be invariably lower than one. A magnetar differs from other rotationally powered pulsars only in that it is observed along a privileged latitudinal direction relative to its spin axis: the closer is the line of sight to a direction in which the radiation from the current sheet is focused, the higher the frequency content and the lower the decay rate with distance of the observed radiation. The outbursts characterizing the emission of a magnetar thus arise from sudden movements of its spin or magnetic axes.
