中子星磁层“闪电”的形成与RRAT的性质
Formation of "Lightnings" in a Neutron Star Magnetosphere and the Nature of RRATs
摘要：
研究了中子星磁层吸收宇宙γ射线背景高能光子产生的“闪电”射电辐射与旋转射电瞬变（RRAT）射电爆发之间的联系。闪电长度达到1000公里;闪电半径为100米，与极冠半径相当。如果一个封闭的磁层充满了致密的等离子体，那么闪电只会在开放的磁场线区域有效地形成。为了观测到来自单独闪电的无线电发射，中子星的极冠必须指向观测者，同时闪电必须形成。最大爆发率与血浆从极帽区流出的时间有关。两个连续脉冲串之间的典型间隔约为100 s。单个射电爆发的宽度可以由中子星表面上方一定高度的闪电发射区形成的发射锥的宽度和有限的闪电寿命决定。来自RRAT的无线电突发的相位分布的宽度以及积分脉冲宽度由无线电发射的形成高度处的开放磁场线束的宽度确定。所获得的结果与目前可用的数据是一致的，并表明RRAT，间歇性的间歇性的，极端零之间的密切联系。
英文摘要：
The connection between the radio emission from "lightnings" produced by the absorption of high-energy photons from the cosmic gamma-ray background in a neutron star magnetosphere and radio bursts from rotating radio transients (RRATs) is investigated. The lightning length reaches 1000 km; the lightning radius is 100 m and is comparable to the polar cap radius. If a closed magnetosphere is filled with a dense plasma, then lightnings are efficiently formed only in the region of open magnetic field lines. For the radio emission from a separate lightning to be observed, the polar cap of the neutron star must be directed toward the observer and, at the same time, the lightning must be formed. The maximum burst rate is related to the time of the plasma outflow from the polar cap region. The typical interval between two consecutive bursts is ~100 s. The width of a single radio burst can be determined both by the width of the emission cone formed by the lightning emitting regions at some height above the neutron star surface and by a finite lightning lifetime. The width of the phase distribution for radio bursts from RRATs, along with the integrated pulse width, is determined by the width of the bundle of open magnetic field lines at the formation height of the radio emission. The results obtained are consistent with the currently available data and are indicative of a close connection between RRATs, intermittent pulsars, and extreme nullers.
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