Nucleosynthesis in Massive Stars with Improved Nuclear and Stellar Physics
Nucleosynthesis in Massive Stars with Improved Nuclear and Stellar Physics
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DOI：
10.1086/341728
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发表时间：
2001-12
期刊：
影响因子：
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通讯作者：
T. Rauscher;A. Heger;R. Hoffman;S. W. B. U. O. Basel;Switzerland.;Ucsc;Usa;U. Chicago;-Llnl
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文献类型：
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作者：
T. Rauscher;A. Heger;R. Hoffman;S. W. B. U. O. Basel;Switzerland.;Ucsc;Usa;U. Chicago;-Llnl
我们提出了第一个遵循所有稳定核的演变及其在爆炸中央氢燃烧的恒星模型中的进化，作为II型超新星的计算。和25m☉使用最近可用的实验和理论核数据，修订的不透明度表，中性损失和弱相互作用率，并考虑了由于恒星风而引起的质量损失。在爆炸期间，核序列的核数（每个时间步骤）范围从主序列上的〜2200不等。恒星质量研究表明，在16o和90zr之间的核能放大器可以达到整体良好的一致性。在核心倒塌之前的一天，我们发现，在倒塌之前，氧气，霓虹灯和碳壳大约在核心崩溃之前，它们仅在爆炸中进行。
We present the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in stellar models computed from the onset of central hydrogen burning through explosion as Type II supernovae. Calculations are performed for Population I stars of 15, 19, 20, 21, and 25 M☉ using the most recently available experimental and theoretical nuclear data, revised opacity tables, neutrino losses, and weak interaction rates and taking into account mass loss due to stellar winds. A novel "adaptive" reaction network is employed with a variable number of nuclei (adjusted each time step) ranging from ~700 on the main sequence to ≳2200 during the explosion. The network includes, at any given time, all relevant isotopes from hydrogen through polonium (Z = 84). Even the limited grid of stellar masses studied suggests that overall good agreement can be achieved with the solar abundances of nuclei between 16O and 90Zr. Interesting discrepancies are seen in the 20 M☉ model and (so far, only in that model) are a consequence of the merging of the oxygen, neon, and carbon shells about a day prior to core collapse. We find that, in some stars, most of the "p-process" nuclei can be produced in the convective oxygen-burning shell moments prior to collapse; in others, they are made only in the explosion. Serious deficiencies still exist in all cases for the p-process isotopes of Ru and Mo.