逆康普顿辐射的偏振特性及其对Blazar GEMS X射线偏振仪观测的意义
The Polarization Properties of Inverse Compton Emission and Implications for Blazar Observations with the GEMS X-Ray Polarimeter
摘要：
定于2014年发射的美国航天局小型探索者任务GEMS（重力和极磁SMEX）将具有探测和测量相当数量的银河系和河外源的0.5千电子伏和2-10千电子伏X射线发射线偏振特性的灵敏度。灵敏的X射线偏振测量的前景证明了更仔细地观察基本发射机制的偏振特性是合理的。在本文中，我们提出的逆康普顿散射辐射的线偏振特性的分析和数值计算。我们描述了一个普遍适用的形式主义，可用于数值计算的汤姆逊和克莱因-西科制度的偏振特性。我们首次使用该程序对数值计算结果和Bonometto等人（1970）在汤姆逊区的散射的早期分析结果进行了详细的比较。此外，我们使用的数值形式主义，以审查同步自康普顿发射的偏振特性，并在克莱因-西名制度发射的逆康普顿辐射。最后，我们讨论了未来GEMS观测耀变体的科学潜力。地球同步监测系统飞行任务将能够确认高频率峰值BL Lac天体低能发射部分的同步辐射源。此外，观察有可能决定之间的同步自康普顿和外部康普顿起源的高能发射分量的平谱射电类星体和低频峰值BL Lac对象。
英文摘要：
NASA's Small Explorer Mission GEMS (Gravity and Extreme Magnetism SMEX), scheduled for launch in 2014, will have the sensitivity to detect and measure the linear polarization properties of the 0.5 keV and 2-10 keV X-ray emission of a considerable number of galactic and extragalactic sources. The prospect of sensitive X-ray polarimetry justifies a closer look at the polarization properties of the basic emission mechanisms. In this paper, we present analytical and numerical calculations of the linear polarization properties of inverse Compton scattered radiation. We describe a generally applicable formalism that can be used to numerically compute the polarization properties in the Thomson and Klein-Nishina regimes. We use the code to perform for the first time a detailed comparison of numerical results and the earlier analytical results derived by Bonometto et al. (1970) for scatterings in the Thomson regime. Furthermore, we use the numerical formalism to scrutinize the polarization properties of synchrotron self-Compton emission, and of inverse Compton radiation emitted in the Klein-Nishina regime. We conclude with a discussion of the scientific potential of future GEMS observations of blazars. The GEMS mission will be able to confirm the synchrotron origin of the low-energy emission component from high frequency peaked BL Lac objects. Furthermore, the observations have the potential to decide between a synchrotron self-Compton and external-Compton origin of the high-energy emission component from flat spectrum radio quasars and low frequency peaked BL Lac objects.
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