核心坍缩超新星核合成和流星星尘颗粒之间的比较：研究镁、铝和铬
Comparison between core-collapse supernova nucleosynthesis and meteoric stardust grains: investigating magnesium, aluminium, and chromium
摘要：
太阳系固体样品中核合成起源的同位素变化已有很好的记录，但这些变化的起源仍然不确定。在原行星盘不同区域形成的材料中观察到的\iso{54} Cr的变异性归因于太阳前富铬氧化物（铬铁矿）颗粒的数量不一，这些颗粒存在于陨石星尘库存中，很可能起源于某种类型的超新星爆炸。为了研究核心坍缩超新星（CCSNe）是否可能是这些颗粒的起源地，我们分析了初始质量为15，20和25 M $_{\odot}$的恒星CCSN模型的产量，以及太阳金属丰度。我们提出了一个广泛的丰富的数据集的铬，镁，铝同位素作为封闭质量的函数。我们发现的情况下，爆炸性C-灰产生的组合物与观察到的\iso{54} Cr/ \iso{52} Cr和\iso{53} Cr/ \iso{52} Cr比以及\iso{50} Cr/ \iso{52} Cr比非常一致。考虑到原子质量为50的信号也可能源自\iso{50} Ti，爆炸性He燃烧的灰烬也与观察到的比率相匹配。此外，太阳系组成的He灰烬（富含Al和Cr，相对于Mg，以模拟铬铁矿颗粒的组成）的材料可能会重现观察到的Mg和Cr异常之间的相关性，而来自C-灰烬的材料并不存在显着的Mg异常以及Cr同位素的变化。在所有情况下，非放射成因的，稳定的镁同位素的变化占主导地位的变化预计从\iso{26}铝。
英文摘要：
Isotope variations of nucleosynthetic origin among Solar System's solid samples are well documented, yet the origin of these variations is still uncertain. The observed variability of \iso{54}Cr among materials formed in different regions of the proto-planetary disk has been attributed to variable amounts of presolar chromium-rich oxide (chromite) grains, which exist within the meteoritic stardust inventory and most likely originated from some type of supernova explosions. To investigate if core-collapse supernovae (CCSNe) could be the site of origin of these grains, we analyse yields of CCSN models of stars with initial mass 15, 20 and 25 M$_{\odot}$, and solar metallicity. We present an extensive abundance data set of the Cr, Mg, and Al isotopes as a function of enclosed mass. We find cases in which the explosive C-ashes produce a composition in good agreement with the observed \iso{54}Cr/\iso{52}Cr and \iso{53}Cr/\iso{52}Cr ratios as well as the \iso{50}Cr/\iso{52}Cr ratios. Taking into account that the signal at atomic mass 50 could also originate from \iso{50}Ti, the ashes of explosive He-burning also match the observed ratios. Addition of material from the He ashes (enriched in Al and Cr relative to Mg to simulate the make-up of chromite grains) to the Solar System composition may reproduce the observed correlation between Mg and Cr anomalies, while material from the C-ashes does not present significant Mg anomalies together with Cr isotopic variations. In all cases, non-radiogenic, stable Mg isotope variations dominate over the variations expected from \iso{26}Al.
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