用multi-TeV γ射线和中微子寻找银河系cosmic ray pevatron
Searching for galactic cosmic ray pevatrons with multi-TeV gamma rays and neutrinos
摘要：
最近HESS在TeV伽马射线中对超新星遗迹壳层的探测证实了超新星遗迹可以作为强大的宇宙射线加速器的理论预测。如果这些天体是银河系宇宙射线的主要来源，那么它们应该将质子和原子核加速到10 ^15 eV或更高，即充当宇宙PeVatron。扩散激波加速模型在一定条件下允许粒子加速到如此高的能量，并逐渐注入星际介质，主要是在残留物演化的Sedov阶段。能量最高的粒子首先被释放，而能量较低的粒子更有效地被限制在壳层中，并在稍后的时期被释放。因此，壳层内的非热粒子的光谱仅在残余物演化的相对较短的时期内延伸到PeV能量。基于这个原因，我们可以预期次级伽马射线和中微子的光谱只有从T \lesssim 1000年前的超新星遗迹中才能延伸到10 TeV以上的能量。另一方面，如果一个巨大的气体云偶然出现在超新星遗迹的\lesssim 100 pc附近，当从超新星壳层出现的最具能量的粒子到达云时，伽马射线和中微子的“延迟”多TeV信号就会出现。这种延迟发射的多TeV伽马射线和中微子的检测允许间接识别超新星遗迹作为粒子PeVatron。
英文摘要：
The recent HESS detections of supernova remnant shells in TeV gamma-rays confirm the theoretical predictions that supernova remnants can operate as powerful cosmic ray accelerators. If these objects are responsible for the bulk of galactic cosmic rays, then they should accelerate protons and nuclei to 10^15 eV and beyond, i.e. act as cosmic PeVatrons. The model of diffusive shock acceleration allows, under certain conditions, acceleration of particles to such high energies and their gradual injection into the interstellar medium, mainly during the Sedov phase of the remnant evolution. The most energetic particles are released first, while particles of lower energies are more effectively confined in the shell, and are released at later epochs. Thus the spectrum of nonthermal paticles inside the shell extends to PeV energies only during a relatively short period of the evolution of the remnant. For this reason one may expect spectra of secondary gamma-rays and neutrinos extending to energies beyond 10 TeV only from T \lesssim 1000 yr old supernova remnants. On the other hand, if by a chance a massive gas cloud appears in the \lesssim 100 pc vicinity of the supernova remnant, ``delayed'' multi-TeV signals of gamma-rays and neutrinos arise when the most energetic partices emerged from the supernova shell reach the cloud. The detection of such delayed emission of multi-TeV gamma-rays and neutrinos allows indirect identification of the supernova remnant as a particle PeVatron.
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