论文标题
Cygnus Cocoon的GEV-TEV伽马射线排放的建模
Modeling of GeV-TeV gamma-ray emission of Cygnus Cocoon
论文作者
论文摘要
在能量基本的银河系强力室中，ob缔合和超级泡沫可能是银河宇宙射线（CRS）的重要加速位点。与超级泡和恒星簇相关的伽马射线源的发射曲线表明，大型恒星的风连续颗粒加速。最发光的银河系伽马射线源之一是Cygnus Cocoon Superbleble，由多种仪器（例如Fermi-Lat，Argo和最近的Hawc）观察到。我们讨论了粒子加速和运输模型，以解释Cygnus Cocoon的GEV-TEV伽马射线光谱，该光谱的能量约为1 TEV。结果表明，高能质子的宽度相互作用产生的伽玛射线是由于Cygnus Cocoon中巨大恒星和超新星风的一系列冲击而加速的，可以解释观察结果。最高能量的质子光谱形状取决于茧中的MHD裂开光谱。 Cygnus Cocoon的可行解决方案可以应用于显示相似行为的其他一些关联。我们简要讨论了延伸的超级泡中粒子加速过程的相似性和差异，以及以Westerlund 1和2 Gamma-ray源代表的年轻大型恒星的紧凑簇簇。
OB-associations and superbubbles being energetically essential galactic powerhouses are likely to be the important acceleration sites of galactic cosmic rays (CRs). The emission profile of gamma-ray sources related to superbubbles and stellar clusters indicates on continuous particle acceleration by winds of massive stars. One of the most luminous galactic gamma-ray sources is Cygnus Cocoon superbubble, observed by multiple instruments, such as Fermi-LAT, ARGO, and, recently, HAWC. We discuss a model of particle acceleration and transport in a superbubble to explain GeV-TeV gamma-ray spectrum of Cygnus Cocoon, which has a break at the energy of about 1 TeV. It is shown that the gamma rays produced by hadronic interactions of high-energy protons accelerated by an ensemble of shocks from winds of massive stars and supernovae in the Cygnus Cocoon can explain the observations. The proton spectral shape at the highest energies depends on the MHD-fluctuation spectrum in the Cocoon. The viable solutions for Cygnus Cocoon may be applied to some other associations showing similar behaviour. We briefly discuss the similarity and differences of particle acceleration processes in extended superbubbles and compact clusters of young massive stars as represented by Westerlund 1 and 2 gamma-ray sources.
