Determination of alpha spectroscopic factors for unbound 17 O states
Determination of alpha spectroscopic factors for unbound 17 O states
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未结合 17 O 状态的 α 光谱因子的测定
DOI：
10.1051/epjconf/201716501022
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发表时间：
2017
影响因子：
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通讯作者：
De Séréville N
中科院分区：
文献类型：
--
作者：
De Séréville N
最近有人提出，当核心坍缩超新星（ccSN）的爆炸穿过大质量恒星的氦壳层时，氢被吸入氦壳层可能导致高13 C和15 N过量。这一预测的问题非常高的13 C和15 N丰度观察到罕见的前太阳SiC颗粒，这通常是由于经典的新星的起源。13 N（α，p）16 O反应与13 N β ~+-衰变为13 C反应竞争，在这方面起着重要的作用。作为确定13 N（α，p）16 O反应速率的第一步，我们研究了17 O态的α谱因子，它与13 N（α，p）16 O反应的复合核17 F的α谱因子类似。
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could lead to high13C and15N excesses when the blast of a core collapse supernova (ccSN) passes through its helium shell. This prediction questions the origin of extremely high13C and15N abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context the13N(α,p)16O reaction plays an important role since it is in competition with13Nβ+-decay to13C. As a first step to the determination of the13N(α,p)16O reaction rate, we present a study aiming at the determination of alpha spectroscopic factors of17O states which are the analog ones to those in17F, the compound nucleus of the13N(α,p)16O reaction.