展望未来：用IR干涉测量法研究微类星体
Looking to the future: using IR interferometry to study microquasars
摘要：
红外干涉测量法目前正处于快速发展阶段，新的仪器很快就能达到微弱光源的毫角秒空间分辨率和10微角秒量级的天体测量分辨率。特别是对于喷流研究，下一代仪器将使我们更接近Sgr A* 等超大质量黑洞的事件视界，以及喷流发射必须发生的区域。但是，利用类似于寻找恒星周围微弱系外行星的技术，也可能出现一种研究微类星体的新可能性，特别是喷流物理学。在硬态X射线双星中观察到的紧凑、稳定的喷流显示出从较低的无线电波长到至少远红外波段的平坦/倒置光谱。在这个波段之上的某个地方，预测会出现一个营业额，在那里射流变得光学薄，揭示了幂律谱。这种破裂可能在GX 339 -4中直接观测到，但在大多数来源中，这种特征可能隐藏在恒星伴星或吸积盘组件的明亮发射下。探测这个断裂的确切位置将为我们的射流物理模型提供一个新的约束，因为断裂频率取决于总功率，以及内部密度和磁场。此外，知道断裂位置结合幂律的光谱指数将有助于限制由喷流贡献的X射线波段的同步辐射量。随着一些潜在的观测需要不太优化的仪器规格的总结，我将讨论一种技术，它可以使我们能够辨别射流中断，以及成功的机会，根据理论模型应用到一些潜在的目标源。
英文摘要：
Infrared interferometry is currently in a rapid development phase, with new instrumentation soon achieving milliarcsecond spatial resolutions for faint sources and astrometry on the order of 10 microarcseconds. For jet studies in particular, the next generation of instruments will bring us closer to the event horizon of supermassive black holes such as Sgr A*, and the region where jet launching must occur. But a new possibility to study microquasars in general and jet physics in particular may also arise, using techniques similar to those employed for finding faint exoplanets around stars. The compact, steady jets observed in the hard state of X-ray binaries display a flat/inverted spectrum from the lower radio wavelengths up through at least the far-IR band. Somewhere above this band, a turnover is predicted where the jets become optically thin, revealing a power-law spectrum. This break may have been observed directly in GX339-4, but in most sources such a feature is likely hidden under bright emission from the stellar companion or accretion disk components. Detecting the exact location of this break would provide a new constraint on our models of jet physics, since the break frequency is dependent on the total power, as well as internal density and magnetic field. Furthermore, knowing the break location combined with the spectral index of the power-law would help constrain the amount of synchrotron emission contributed by the jets to the X-ray bands. Along with a summary of some potential observations requiring less optimal instrumental specifications, I will discuss a technique which may enable us to discern the jet break, and the chances of success based on theoretical models applied to some potential target sources.
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