The origins of the elements and isotopes of cosmic material is a critical aspect of understanding the evolution of the universe. Nucleosynthesis typically requires physical conditions of high temperatures and densities. These are found in the Big Bang, in the interiors of stars, and in explosions with their compressional shocks and high neutrino and neutron fluxes. Many different tools are available to disentangle the composition of cosmic matter, in material of extraterrestrial origins such as cosmic rays, meteorites, stardust grains, lunar and terrestrial sediments, and through astronomical observations across the electromagnetic spectrum. Understanding cosmic abundances and their evolution requires combining such measurements with approaches of astrophysical, nuclear theories and laboratory experiments, and exploiting additional cosmic messengers, such as neutrinos and gravitational waves. Recent years have seen significant progress in almost all these fields; they are presented in this review.

The Sun and the solar system are our reference system for abundances of elements and isotopes. Many direct and indirect methods are employed to establish a refined abundance record from the time when the Sun and the Earth were formed. Indications for nucleosynthesis in the local environment when the Sun was formed are derived from meteoritic material and inclusion of radioactive atoms in deep-sea sediments. Spectroscopy at many wavelengths and the neutrino flux from the hydrogen fusion processes in the Sun have established a refined model of how the nuclear energy production shapes stars. Models are required to explore nuclear fusion of heavier elements. These stellar evolution calculations have been confirmed by observations of nucleosynthesis products in the ejecta of stars and supernovae, as captured by stardust grains and by characteristic lines in spectra seen from these objects. One of the successes has been to directly observe $\gamma$ rays from radioactive material synthesised in stellar explosions, which fully support the astrophysical models. Another has been the observation of radioactive afterglow and characteristic heavy-element spectrum from a neutron-star merger, confirming the neutron rich environments encountered in such rare explosions. The ejecta material captured by Earth over millions of years in sediments and identified through characteristic radio-isotopes suggests that nearby nucleosynthesis occurred in recent history, with further indications for sites of specific nucleosynthesis. Together with stardust and diffuse $\gamma$ rays from radioactive ejecta, these help to piece together how cosmic materials are transported in interstellar space and re-cycled into and between generations of stars. Our description of cosmic compositional evolution needs such observational support, as it rests on several assumptions that appear challenged by recent recognition of violent events being common during evolution of a galaxy. This overview presents the flow of cosmic matter and the various sites of nucleosynthesis, as understood from combining many techniques and observations, towards the current knowledge of how the universe is enriched with elements.

宇宙物质元素和同位素的起源是理解宇宙演化的一个关键方面。核合成通常需要高温和高密度的物理条件。这些存在于大爆炸、恒星内部，以及带有压缩冲击和高中微子和中子通量的爆炸中。许多不同的工具可用于解开宇宙物质的组成，包括来自外星的物质，如宇宙射线、陨石、星尘颗粒、月球和陆地沉积物，以及通过电磁波谱的天文观测。了解宇宙丰度及其演化需要将此类测量与天体物理学、核理论和实验室实验的方法相结合，并利用额外的宇宙信使，例如中微子和引力波。近年来，几乎所有这些领域都取得了重大进展；它们在本次审查中介绍。

太阳和太阳系是我们丰富元素和同位素的参考系统。从太阳和地球形成的那一刻起，许多直接和间接的方法被用来建立一个精确的丰度记录。太阳形成时在当地环境中进行核合成的迹象来自陨石物质和深海沉积物中包含的放射性原子。许多波长的光谱学和来自太阳氢聚变过程的中微子通量已经建立了核能产生如何塑造恒星的精细模型。需要模型来探索较重元素的核聚变。这些恒星演化计算已通过对恒星和超新星喷射中的核合成产物的观察得到证实，由星尘颗粒和从这些物体看到的光谱中的特征线捕获。成功之一是直接观察$\gamma$ 恒星爆炸中合成的放射性物质发出的射线，完全支持天体物理模型。另一个是对中子星合并的放射性余辉和特征重元素光谱的观察，证实了在这种罕见的爆炸中遇到的富含中子的环境。地球在沉积物中捕获了数百万年并通过特征放射性同位素识别的喷射物质表明，附近的核合成发生在近代历史上，并进一步表明了特定核合成的地点。与星尘一起弥漫$\gamma$ 来自放射性喷射物的射线，这些有助于拼凑宇宙物质如何在星际空间中运输，以及如何在几代恒星之间重新循环。我们对宇宙成分演化的描述需要这样的观测支持，因为它基于几个假设，这些假设似乎受到最近对星系演化过程中常见的暴力事件的认识的挑战。本概述介绍了宇宙物质的流动和核合成的各个部位，通过结合许多技术和观察来理解，以了解当前关于宇宙如何富含元素的知识。