强场对脉冲星到达时间的影响：圆形轨道和赤道波束
Strong field effects on pulsar arrival times: circular orbits and equatorial beams
摘要：
如果一颗脉冲星围绕着一个超大质量黑洞运行，那么通过黑洞附近的脉冲的时间将显示出各种各样的强场效应。为了计算接近非旋转黑洞的脉冲的强度和时间，我们在这里引入一个简单的形式主义，基于两个“通用函数”，一个是光子轨迹的弯曲，另一个是光子在这些轨迹上的旅行时间。我们应用这个简单的形式主义的情况下，脉冲星在圆形轨道上的光束进入轨道平面的脉冲。除了通过或多或少的直接路径到达接收器的“初级”脉冲之外，我们发现存在次级和高阶脉冲。这些脉冲通常比主脉冲暗得多，但如果脉冲星在离接收器最远的黑洞一侧发射，它们的强度可以相当，甚至更大。我们表明，有一个相位关系的主要和次要的脉冲，这是一个探针的强烈弯曲的时空几何。在更一般的配置中，这些现象的类似物是可以预期的，在这种配置中，围绕黑洞轨道的脉冲星发出的脉冲不限于轨道平面。
英文摘要：
If a pulsar orbits a supermassive black hole, the timing of pulses that pass close to the hole will show a variety of strong field effects. To compute the intensity and timing of pulses that have passed close to a nonrotating black hole we introduce here a simple formalism based on two "universal functions," one for the bending of photon trajectories and the other for the photon travel time on these trajectories. We apply this simple formalism to the case of a pulsar in circular orbit that beams its pulses into the orbital plane. In addition to the "primary" pulses that reach the receiver by a more-or-less direct path, we find that there are secondary and higher order pulses. These are usually much dimmer than the primary pulses, but they can be of comparable or even greater intensity if they are emitted when pulsar is on the side of the hole furthest from the receiver. We show that there is a phase relationship of the primary and secondary pulses that is a probe of the strongly curved spacetime geometry. Analogs of these phenomena are expected in more general configurations, in which a pulsar in orbit around a hole emits pulses that are not confined to the orbital plane.
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