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Determining nucleosynthesis yields in supernovae with spectral modelling

机译:用光谱造型确定超新月的核酸核酸产量

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The methodology to estimate element masses in supernova ejecta from nebular spectroscopy is discussed. Results using the SUMO spectral synthesis code are reviewed with regard to two key elements; oxygen (a hydrostatic burning ash) and nickel (an explosive burning ash). The typical oxygen mass in both Type IIP and IIb supernovae is found to be~0.5 M_⊙, and points to progenitor stars in the 8-17 M_⊙ range. For nickel, a new diagnostic method has been developed that shows Ni/Fe production close to solar in most cases, but sometimes larger by a factor of a few. It is shown that the larger values require the burning of silicon shell layers in the progenitor, a unique constraint on explosion theory.
机译:讨论了从内脏光谱中估计超新墨喷射物元素肿块的方法。 关于两个关键要素审查了使用Sumo谱综合代码的结果; 氧气(静液压燃烧灰)和镍(爆炸性燃烧灰)。 发现IIP和IIB Supernovae两种典型的氧气被发现为〜0.5m,并且指向8-17m_⊙范围内的祖恒星。 对于镍,已经开发了一种新的诊断方法,在大多数情况下,显示了靠近太阳的Ni / Fe产量,但有时略大一倍。 结果表明,较大的值需要在祖先的血液壳层中燃烧,对爆炸理论的独特约束。

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