论文标题
重复由小体绕脉冲星或磁铁引起的快速无线电爆发
Repeating fast radio bursts caused by small bodies orbiting a pulsar or a magnetar
论文作者
论文摘要
旋转到高度磁化和高度相对论风的小行星为重复快速无线电爆发（FRB）提供了有利的配置。与风直接接触的身体形成了一条由固定的alfvén波形成的步道，称为\ textit {alfvénWing}。当风的元素越过Alfvén机翼时，它看到环境磁场的旋转可能导致无线电波不稳定性。在观察者的参考框架中，波浪以非常狭窄的方向范围进行准确，并且强度极高。一项以前出版的作品于2014年发表，表明，旋转脉冲星的行星会在我们的视线中传递时会导致FRB。我们预测了周期性的FRB。从那时起，就发现了随机的FRB中继器。 我们提出了该理论的升级，其中较小的身体与脉冲星风的相互作用可以解释中继器。 考虑到脉冲星风中附着在身体上的相对论alfvén机翼的特性，并考虑到热考虑，我们进行了一项参数研究。 我们发现，包括Lorimer Burst（30 JY）在内的FRB可以通过从高度磁化的毫秒的脉冲星之间的0.03和1 au之间的小型脉冲星（1至10 km）来解释。一些参数也与磁力兼容。我们的模型与FRB121102的高旋转度量兼容。 FRB的束时是中等风湍流的结果。由于由少于200具尸体组成的小行星带对于用FRB121102测量的FRB发生率就足够了。 此模型在当前升级后，与自2014年首次出版物以来发现的属性兼容，当时重复FRB仍然未知。它基于标准物理学以及可以在任何类型的星系中找到的常见天体物理对象。它需要$ 10^{10} $倍的$倍的功率，比（常见）各向同性发射FRB型号。
Asteroids orbiting into the highly magnetized and highly relativistic wind of a pulsar offer a favourable configuration for repeating fast radio bursts (FRB). The body in direct contact with the wind develops a trail formed of a stationary Alfvén wave, called an \textit{Alfvén wing}. When an element of wind crosses the Alfvén wing, it sees a rotation of the ambient magnetic field that can cause radio-wave instabilities. In the observer's reference frame, the waves are collimated in a very narrow range of directions, and they have an extremely high intensity. A previous work, published in 2014, showed that planets orbiting a pulsar can cause FRB when they pass in our line of sight. We predicted periodic FRB. Since then random FRB repeaters have been discovered. We present an upgrade of this theory where repeaters can be explained by the interaction of smaller bodies with a pulsar wind. Considering the properties of relativistic Alfvén wings attached to a body in the pulsar wind, and taking thermal consideration into account we conduct a parametric study. We find that FRBs, including the Lorimer burst (30 Jy), can be explained by small size pulsar companions (1 to 10 km) between 0.03 and 1 AU from a highly magnetized millisecond pulsar. Some sets of parameters are also compatible with a magnetar. Our model is compatible with the high rotation measure of FRB121102. The bunched timing of the FRBs is the consequence of a moderate wind turbulence. As asteroid belt composed of less than 200 bodies would suffice for the FRB occurrence rate measured with FRB121102. This model, after the present upgrade, is compatible with the properties discovered since its first publication in 2014, when repeating FRB were still unknown. It is based on standard physics, and on common astrophysical objects that can be found in any kind of galaxy. It requires $10^{10}$ times less power than (common) isotropic-emission FRB models.
