论文标题
定期活跃快速无线电爆发源的中子星白矮人二进制模型
A Neutron Star-White Dwarf Binary Model for Periodically Active Fast Radio Burst Sources
论文作者
论文摘要
我们提出了一个带有偏心轨道的紧凑型二进制模型，以解释周期性的快速无线电爆发（FRB）源，该系统由具有强偶性磁场和磁性白矮人（WD）组成的中子星（NS）组成。在我们的模型中，WD在Periastron处填充了其Roche Lobe，从WD到NS周围的NS发生质量。积聚的材料可能会分散成许多部分，它们在不同时间到达NS。碎片化的材料可能会触发NS表面附近的磁重新连接。电子可以加速到超偏好的速度，因此电子的曲率辐射可以解释爆发活性。在这种情况下，爆发活动的占空比与二进制的轨道时期有关。我们表明，这样的模型可能会在大约十分钟到两天的时间内为税收周期工作。对于最近报道的FRB 180916.J0158+65的16.35天周期性，我们的模型并不能自然地解释如此长的占空比周期，因为需要极高的偏心率（$ e> 0.95 $）。
We propose a compact binary model with an eccentric orbit to explain periodically active fast radio burst (FRB) sources, where the system consists of a neutron star (NS) with strong dipolar magnetic fields and a magnetic white dwarf (WD). In our model, the WD fills its Roche lobe at periastron, and mass transfer occurs from the WD to the NS around this point. The accreted material may be fragmented into a number of parts, which arrive at the NS at different times. The fragmented magnetized material may trigger magnetic reconnection near the NS surface. The electrons can be accelerated to an ultra-relativistic speed, and therefore the curvature radiation of the electrons can account for the burst activity. In this scenario, the duty cycle of burst activity is related to the orbital period of the binary. We show that such a model may work for duty cycles roughly from ten minutes to two days. For the recently reported 16.35-day periodicity of FRB 180916.J0158+65, our model does not naturally explain such a long duty cycle, since an extremely high eccentricity ($e>0.95$) is required.
