猎户座四边形星团内大质量恒星$Θ^1$ Ori C的激波风中电子的低效加速
Inefficient acceleration of electrons in the shocked wind of the massive star $Θ^1$ Ori C within the Trapezium cluster
AI总结：
本研究针对猎户座四边形星团中$Θ^1$ Ori C激波风的电子加速过程展开，通过时变模型分析发现能量转换效率极低时其伽马辐射符合现有观测，且未来仅能被CTA勉强探测。
摘要：
年轻星团中大质量恒星的激波风被认为是相对论粒子可能的加速场所。在这类环境中加速的电子，预计会有效康普顿化（来自大质量恒星的）光学辐射以及（被星团内尘埃再次散射的）红外辐射，从而产生GeV-TeV伽马射线。我们研究了猎户座四边形（Trapezium）星团内大质量恒星$Θ^1$ Ori C的恒星风中电子的加速、传播和辐射的时变过程，该星团位于邻近的猎户座大星云（M 42）内。我们的研究表明，只要恒星风向相对论电子的能量转换效率极低，即$χ< 10^{-4}$，那么猎户座四边形星团预期产生的伽马射线辐射就与费米大面积望远镜（Fermi-LAT）目前对猎户座分子云的观测结果一致。在如此低的效率下，由$Θ^1$ Ori C恒星风中加速的电子产生的伽马射线辐射，未来仅能被切伦科夫望远镜阵列（Cherenkov Telescope Array，CTA）等切伦科夫望远镜勉强观测到。
英文摘要：
Shocked winds of massive stars in young stellar clusters have been proposed as possible sites in which relativistic particles are accelerated. Electrons, accelerated in such an environment, are expected to efficiently comptonize optical radiation (from massive stars) and the infra-red radiation (re-scattered by the dust within the cluster) producing GeV-TeV gamma-rays. We investigate the time dependent process of acceleration, propagation and radiation of electrons in the stellar wind of the massive star $Θ^1$ Ori C within the Trapezium cluster. This cluster is located within the nearby Orion Nebula (M 42). We show that the gamma-ray emission expected from the Trapezium cluster is consistent with the present observations of the Orion Molecular Cloud by the Fermi-LAT telescope provided that the efficiency of energy conversion from the stellar wind to relativistic electrons is very low, i.e. $χ< 10^{-4}$. For such low efficiencies, the gamma-ray emission from electrons accelerated in the stellar wind of $Θ^1$ Ori C can be only barely observed by the future Cherenkov telescopes, e.g. the Cherenkov Telescope Array (CTA).
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