利用电离光谱寻找天体电子偶素
The Search for Celestial Positronium via the Recombination Spectrum
摘要：
正电子素是由束缚的电子-正电子对组成的短寿命原子。在三重态中，当两个粒子的自旋平行时，辐射复合线将在湮灭之前发射。天体正电子偶素的存在是通过对它的湮灭产物的伽马射线观测而揭示的。然而，这些观测具有固有的低角分辨率。在本文中，我们审查的前景检测的正电子素复合谱。这种观测有可能首次揭示正电子的离散源，并将使光学望远镜和仪器的敏锐度应用于高能现象的观测。我们回顾了正电子素复合谱的理论，并提供了公式来计算预期的线强度的正电子产生率和不同的条件下，在星际介质。我们估计了几类银河系和河外源的正电子偶素发射线强度。这些是比较目前的观测极限和当前和未来的光学和红外仪器的灵敏度。我们发现，由于近红外光谱学的最新进展，PS-α线的观测应该很快成为可能。
英文摘要：
Positronium is the short-lived atom consisting of a bound electron-positron pair. In the triplet state, when the spins of both particles are parallel, radiative recombination lines will be emitted prior to annihilation. The existence of celestial positronium is revealed through gamma-ray observations of its annihilation products. These observations however have intrinsically low angular resolution. In this paper we examine the prospects for detecting the positronium recombination spectrum. Such observations have the potential to reveal discrete sources of positrons for the first time and will allow the acuity of optical telescopes and instrumentation to be applied to observations of high energy phenomena. We review the theory of the positronium recombination spectrum and provide formulae to calculate expected line strengths from the positrons production rate and for different conditions in the interstellar medium. We estimate the positronium emission line strengths for several classes of Galactic and extragalactic sources. These are compared to current observational limits and to current and future sensitivities of optical and infrared instrumentation. We find that observations of the Ps-alpha line should soon be possible due to recent advances in near-infrared spectroscopy.
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