论文标题
宇宙射线修饰冲击的动力学模拟II：粒子光谱
Kinetic Simulations of Cosmic-Ray-Modified Shocks II: Particle Spectra
论文作者
论文摘要
扩散冲击加速度是在空间和天体物理系统中产生能量颗粒的重要机制。长期以来，这种能量颗粒已被预测会影响冲击的流体动力结构，进而导致CR光谱比测试粒子预测更平坦。然而，在这项工作中，与同伴论文，C。C。C. Haggerty和D. Caprioli，2020年，Arxiv：2008.12308 [Astro-Ph.he]，我们使用自洽的混合动力车（动离氟电子）模拟，以首次显示CR-Sodifiend Soptifiend的冲击实际上产生陡峭的陡峭光谱。陡峭的趋势是由嵌入在冲击下游磁性湍流的CR的增强驱动的，我们称为“后人”。这些结果与超新星和超新星残留物的多波长观察结果一致，并且对空间/天体物理冲击具有显着的现象学意义。
Diffusive shock acceleration is a prominent mechanism for producing energetic particles in space and in astrophysical systems. Such energetic particles have long been predicted to affect the hydrodynamic structure of the shock, in turn leading to CR spectra flatter than the test-particle prediction. However, in this work along with a companion paper, C. C. Haggerty and D. Caprioli, 2020, arXiv:2008.12308 [astro-ph.HE], we use self-consistent hybrid (kinetic ions-fluid electrons) simulations to show for the first time how CR-modified shocks actually produce steeper spectra. The steepening is driven by the enhanced advection of CRs embedded in magnetic turbulence downstream of the shock, in what we call the "postcursor". These results are consistent with multi-wavelength observations of supernovae and supernova remnants and have significant phenomenological implications for space/astrophysical shocks in general.
