标题： 宇宙射线相互作用与化学元素的丰度 显示英文标题

标题： Cosmic Ray Interactions and the Abundances of the Chemical Elements

摘要： 我们的银河系是已知最大的核相互作用实验，因为宇宙射线粒子与星际物质之间的相互作用。 宇宙射线是由银河系或星外空间加速的粒子。 宇宙射线以质子、电子、较重的原子核及其反粒子的形式存在。 对于一些高达几十TeV粒子能量的情况，可以推导出宇宙射线的化学丰度。 有人提出，宇宙射线粒子可以归因于三个主要的起源和加速地点：a) 星际介质中的超新星激波，b) 原始恒星风中的超新星激波，c) 强大的射电星系。 这一提议导致了定量测试，迄今为止这些测试令人鼓舞。 关于传输和相互作用的定量模型似乎与数据一致。 在宇宙射线中，Li、Be、B以及许多奇数Z元素和亚铁元素都是次级元素。 在非常低的能量下，宇宙射线粒子受到电离损失的影响，这会产生一个陡峭的低能截止；所有低于截止值的粒子都被移入热物质群体，而高于此值的粒子则仍保留为宇宙射线。 这改变了星际介质中的化学丰度，并且是许多Li、Be、B同位素的主要过程。 提出了宇宙射线起源的定量理论后，寻找更好的裂变截面似乎是有价值的，尤其是在阈值附近。 有了这样改进的一组截面，星际介质及其在热粒子和高能粒子中的化学丰度的理论可以迈出一大步。 显示英文摘要

摘要： Our Galaxy is the largest nuclear interaction experiment which we know, because of the interaction between cosmic ray particles and the interstellar material. Cosmic rays are particles, which have been accelerated in the Galaxy or in extragalactic space. Cosmic rays come as protons, electrons, heavier nuclei, and their antiparticles. Up to energies up to some tens of TeV of particle energy it is possible to derive chemical abundances of cosmic rays. It has been proposed that cosmic ray particles can be attributed to three main sites of origin and acceleration, a) supernova shocks in the interstellar medium, b) supernova shocks in a stellar wind of the predecessor star, and c) powerful radio galaxies. This proposal leads to quantitative tests, which are encouraging sofar. Quantitative models for transport and interaction appear to be consistent with the data. Li, Be, B are secondary in cosmic rays, as are many of the odd-Z elements, as well as the sub-Fe elements. At very low energies, cosmic ray particles are subject to ionization losses, which produce a steep low energy cutoff; all particles below the cutoff are moved into the thermal material population, and the particles above it remain as cosmic rays. This then changes the chemical abundances in the interstellar medium, and is a dominant process for many isotopes of Li, Be, B. With a quantitative theory for the origin of cosmic rays proposed, it appears worthwhile to search for yet better spallation cross sections, especially near threshold. With such an improved set of cross sections, the theory of the interstellar medium and its chemical abundances, both in thermal and in energetic particles, could be taken a large step forward.