Liu Nan, Lugaro Maria, Leitner Jan, Meyer Bradley S, Schönbächler Maria
Institute for Astrophysical Research, Boston University, Boston, MA 02215 USA.
Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17., H-1121 Budapest, Hungary.
Space Sci Rev. 2024;220(8):88. doi: 10.1007/s11214-024-01122-w. Epub 2024 Nov 12.
We provide an overview of the isotopic signatures of presolar supernova grains, specifically focusing on Ti-containing grains with robustly inferred supernova origins and their implications for nucleosynthesis and mixing mechanisms in supernovae. Recent technique advancements have enabled the differentiation between radiogenic (from Ti decay) and nonradiogenic Ca excesses in presolar grains, made possible by enhanced spatial resolution of Ca-Ti isotope analyses with the Cameca NanoSIMS (Nano-scale Secondary Ion Mass Spectrometer) instrument. Within the context of presolar supernova grain data, we discuss () the production of Ti in supernovae and the impact of interstellar medium heterogeneities on the galactic chemical evolution of Ca/Ca, () the nucleosynthesis processes of neutron bursts and explosive H-burning in Type II supernovae, and () challenges in identifying the progenitor supernovae for Cr-rich presolar nanospinel grains. Drawing on constraints and insights derived from presolar supernova grain data, we also provide an overview of our current understanding of the roles played by various supernova types - including Type II, Type Ia, and electron capture supernovae - in accounting for the diverse array of nucleosynthetic isotopic variations identified in bulk meteorites and meteoritic components. We briefly overview the potential mechanisms that have been proposed to explain these nucleosynthetic variations by describing the transport and distribution of presolar dust carriers in the protoplanetary disk. We highlight existing controversies in the interpretation of presolar grain data and meteoritic nucleosynthetic isotopic variations, while also outlining potential directions for future research.
我们概述了前太阳超新星颗粒的同位素特征，特别关注具有可靠推断超新星起源的含钛颗粒及其对超新星核合成和混合机制的影响。最近的技术进步使得能够区分前太阳颗粒中放射性（来自钛衰变）和非放射性钙过量，这是通过使用Cameca纳米二次离子质谱仪（Nano-scale Secondary Ion Mass Spectrometer）提高钙钛同位素分析的空间分辨率实现的。在前太阳超新星颗粒数据的背景下，我们讨论了：（）超新星中钛的产生以及星际介质不均匀性对钙/钙银河化学演化的影响；（）II型超新星中中子爆发和爆发性氢燃烧的核合成过程；（）识别富含铬的前太阳纳米尖晶石颗粒的前身超新星所面临的挑战。利用从前太阳超新星颗粒数据中获得的限制和见解，我们还概述了我们目前对各种超新星类型——包括II型、Ia型和电子俘获超新星——在解释在大块陨石和陨石成分中发现的各种核合成同位素变化所起作用的理解。我们通过描述前太阳尘埃载体在原行星盘中的传输和分布，简要概述了为解释这些核合成变化而提出的潜在机制。我们强调了在前太阳颗粒数据和陨石核合成同位素变化解释方面存在的争议，同时也概述了未来研究的潜在方向。
