Particle Acceleration in the Cygnus Superbubble
Particle Acceleration in the Cygnus Superbubble
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DOI：
10.22323/1.395.0831
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发表时间：
2021-07
期刊：
影响因子：
--
通讯作者：
B. Hona
中科院分区：
文献类型：
--
作者：
B. Hona
天鹅座茧是第一个伽马射线超级气泡，由一个巨大的恒星协会--OB2协会提供动力。据推测，OB2协会的所有大质量O型恒星的恒星风的综合效应可以加速宇宙射线在茧中转化为PeV能量。在茧中加速到PeV能量的确凿证据将确定恒星的关联是PeV宇宙线加速器，即PeVatron。然而，此前对蚕茧的研究只有10TeV以下。在这项贡献中，利用1343天的高海拔水切伦科夫(HAWC)观测数据，我们提出了从1TeV以上到100TeV以上的蚕茧的形态和光谱研究。在较高TeV能量下的分析显示，与GeV伽马射线观测相比，光谱较软。这一结果表明，加速器的效率在数百TeV左右下降，或者在被加速后，最高能量的质子逃离该区域。这里介绍的10TeV以上的研究展示了CR加速器如何在这些极端能量下运行，以及粒子传输如何影响高能发射。
The Cygnus Cocoon is the first gamma-ray superbubble powered by a massive stellar association, the OB2 association. It was postulated that the combined effects of the stellar winds of all the massive O-type stars of the OB2 association can accelerate the cosmic rays to PeV energy in the Cocoon. The conclusive proof of acceleration to PeV energy in the Cocoon will identify the stellar association as a PeV cosmic-ray accelerator, known as PeVatron. However, the Cocoon has been previously studied only up to 10 TeV. In this contribution, using 1343 days of High Altitude Water Cherenkov (HAWC) observatory data, we present the morphological and spectral study of the Cocoon above 1 TeV to beyond 100 TeV. The analysis at higher TeV energies reveals a softer spectrum compared to the GeV gamma-ray observation. This result suggests that the accelerator’s efficiency decreases around hundreds of TeV, or after being accelerated, the highest-energy protons escape the region. The study above 10 TeV presented here demonstrates how CR accelerators operate in these extreme energies and how particle transport impacts high-energy emission.