We present the status and open problems of nucleosynthesis in supernova explosions of both types, responsible for the production of the intermediate mass, Fe-group and heavier elements (with the exception of the main s-process). Constraints from observations can be provided through individual supernovae (SNe) or their remnants (e.g. via spectra and gamma-rays of decaying unstable isotopes) and through surface abundances of stars which witness the composition of the interstellar gas at their formation. With a changing fraction of elements heavier than He in these stars (known as metallicity) the evolution of the nucleosynthesis in galaxies over time can be determined. A complementary way, related to gamma-rays from radioactive decays, is the observation of positrons released in β+$\beta^{+}$-decays, as e.g. from Al26$^{26}\mbox{Al}$, Ti44$^{44}\mbox{Ti}$, Ni56,57$^{56,57}\mbox{Ni}$ and possibly further isotopes of their decay chains (in competition with the production of e+e−$e^{+}e^{-}$ pairs in acceleration shocks from SN remnants, pulsars, magnetars or even of particle physics origin). We discuss (a) the role of the core-collapse supernova explosion mechanism for the composition of intermediate mass, Fe-group (and heavier?) ejecta, (b) the transition from neutron stars to black holes as the final result of the collapse of massive stars, and the relation of the latter to supernovae, faint supernovae, and gamma-ray bursts/hypernovae, (c) Type Ia supernovae and their nucleosynthesis (e.g. addressing the Mn55$^{55}\mbox{Mn}$ puzzle), plus (d) further constraints from galactic evolution, γ$\gamma$-ray and positron observations. This is complemented by the role of rare magneto-rotational supernovae (related to magnetars) in comparison with the nucleosynthesis of compact binary mergers, especially with respect to forming the heaviest r-process elements in galactic evolution.

中文翻译：

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超新星中的核合成

我们介绍了两种类型超新星爆炸中核合成的现状和未解决的问题，负责产生中等质量、Fe 族和较重元素（主 s 过程除外）。观测的约束可以通过单个超新星 (SN) 或其残余物（例如，通过衰变不稳定同位素的光谱和伽马射线）以及通过恒星的表面丰度来提供，这些恒星见证了星际气体在其形成时的成分。随着这些恒星中比 He 重的元素比例发生变化（称为金属丰度），可以确定星系中核合成随时间的演变。与放射性衰变产生的伽马射线相关的一种补充方式是观察 β+$\beta^{+}$-衰变中释放的正电子，例如来自 Al26$^{26}\mbox{Al}$，Ti44$^{44}\mbox{Ti}$, Ni56,57$^{56,57}\mbox{Ni}$ 以及它们衰变链的可能进一步同位素（与 e+e−$e 的产生竞争^{+}e^{-}$ 对来自超新星遗迹、脉冲星、磁星甚至粒子物理起源的加速冲击）。我们讨论（a）核心坍缩超新星爆炸机制对中间质量、Fe 族（和更重的？）喷射物的组成的作用，（b）作为坍缩的最终结果，从中子星到黑洞的转变大质量恒星，以及后者与超新星、微弱超新星和伽马射线爆发/超新星的关系，(c) Ia 型超新星及其核合成（例如解决 Mn55$^{55}\mbox{M​​n}$ 难题)，加上 (d) 来自星系演化、γ$\gamma$ 射线和正电子观测的进一步限制。