THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE
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DOI：
10.1088/0004-637x/810/2/109
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发表时间：
2015-01
期刊：
影响因子：
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通讯作者：
N. Nishimura;T. Takiwaki;Friedrich-Karl Thielemann
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作者：
N. Nishimura;T. Takiwaki;Friedrich-Karl Thielemann
研究了核心坍缩超新星（CC-SNe）中的r过程核合成，重点讨论了旋转和强磁场引起的爆炸情形。核合成计算进行磁流体动力学爆炸模型的基础上，具有广泛的初始旋转和磁场的参数。爆炸模型可分为两类：缓磁喷流和缓磁喷流，这两类模型的原中子星在坍缩和核反弹时的磁场分别较强和相对较弱。根据每个爆炸模型的流体动力学轨迹，我们证实了r-过程成功地发生在非线性磁喷流中，它产生了包括锕系元素在内的重核。另一方面，延迟磁喷流中的r过程被抑制，其仅合成第二峰（A = 130？> ).因此，延迟磁喷流中的r过程只能解释在贫金属恒星中观察到的“弱r过程”模式，而不能解释太阳丰度所代表的“主r过程”。我们的研究结果表明，CC-SNe是可能的重r过程元素的天文源，如果它们的磁场足够强，而较弱的磁爆炸可能产生“弱r过程”图案（A 130？> ).我们显示了潜在的重要性和必要性的磁旋转SNe解释银河系的化学演化，以及丰富的r-过程增强贫金属星。我们还研究了剩余的不确定性的性质的PNS由于弱相互作用，确定最终的中子丰富的喷出物的影响。此外，我们简要讨论了初级射流中的放射性同位素产率（例如，56 Ni）的一些光学观测和相关的高能天文现象。
The r-process nucleosynthesis in core-collapse supernovae (CC-SNe) is studied, with a focus on the explosion scenario induced by rotation and strong magnetic fields. Nucleosynthesis calculations are conducted based on magneto-hydrodynamical explosion models with a wide range of parameters for initial rotation and magnetic fields. The explosion models are classified in two different types: prompt-magnetic-jet and delayed-magnetic-jet, for which the magnetic fields of proto-neutron stars (PNSs) during collapse and the core-bounce are strong and comparatively moderate, respectively. Following the hydrodynamical trajectories of each explosion model, we confirmed that r-processes successfully occur in the prompt-magnetic-jets, which produce heavy nuclei including actinides. On the other hand, the r-process in the delayed-magnetic-jet is suppressed, which synthesizes only nuclei up to the second peak ( A ∼ 130 ?> ). Thus, the r-process in the delayed-magnetic-jets could explain only “weak r-process” patterns observed in metal-poor stars rather than the “main r-process,” represented by the solar abundances. Our results imply that CC-SNe are possible astronomical sources of heavy r-process elements if their magnetic fields are strong enough, while weaker magnetic explosions may produce “weak r-process” patterns ( A ≲ 130 ?> ). We show the potential importance and necessity of magneto-rotational SNe for explaining the galactic chemical evolution, as well as abundances of r-process enhanced metal-poor stars. We also examine the effects of the remaining uncertainties in the nature of PNSs due to weak interactions that determine the final neutron-richness of ejecta. Additionally, we briefly discuss radioactive isotope yields in primary jets (e.g., 56Ni), with relation to several optical observation of SNe and relevant high-energy astronomical phenomena.