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Spectroscopy ofP30and the abundance ofSi29in presolar grains
Physical Review C ( IF 3.2 ) Pub Date : 2020-09-22 , DOI: 10.1103/physrevc.102.035804 G. Lotay , D. T. Doherty , D. Seweryniak , M. P. Carpenter , R. V. F. Janssens , J. José , A. M. Rogers , P. J. Woods , S. Zhu
Physical Review C ( IF 3.2 ) Pub Date : 2020-09-22 , DOI: 10.1103/physrevc.102.035804 G. Lotay , D. T. Doherty , D. Seweryniak , M. P. Carpenter , R. V. F. Janssens , J. José , A. M. Rogers , P. J. Woods , S. Zhu
The astrophysical ) reaction is expected to play a key role in determining the final yields ejected in nova explosions. Such yields are used to accurately identify the stellar origins of meteoritic stardust and recently, distinctive silicon isotopic ratios have been extracted from a number of presolar grains. Here, the light-ion ) fusion-evaporation reaction was used to populate low-spin proton-unbound excited states in the nucleus that govern the rate of the astrophysical ) reaction. In particular, decays were observed from resonances up to , and key resonances at 217 and 315 keV have now been identified as and levels, respectively. The present paper provides the first estimate of the 217-keV resonance strength and indicates that the strength of the 315-keV resonance, which dominates the rate of the ) reaction over the entire peak temperature range of oxygen-neon novae, is higher than previously expected. As such, the abundance of ejected during nova explosions is likely to be less than that predicted by the most recent theoretical models.
中文翻译:
太阳前晶粒中P30的光谱和Si29的丰度
天体物理学 )反应预计将在确定最终结果中发挥关键作用 在新星爆炸中喷出的能量。这样的产量可用于准确识别陨石星尘的恒星起源,近来,已经从许多前太阳晶粒中提取出独特的硅同位素比。在这里,光离子)融合蒸发反应用于填充核中低旋质子未结合的激发态 决定天体物理速率的 )反应。尤其是, 从共振到 ,现在已确定在217和315 keV处的关键共振为 和 级别。本文提供了217-keV共振强度的第一个估计值,并指出315-keV共振的强度决定了共振频率。)在氧氖新星的整个峰值温度范围内的反应比以前预期的要高。因此,丰富的 在新星爆炸期间喷出的水可能比最新理论模型所预测的要少。
更新日期:2020-09-23
中文翻译:
太阳前晶粒中P30的光谱和Si29的丰度
天体物理学 )反应预计将在确定最终结果中发挥关键作用 在新星爆炸中喷出的能量。这样的产量可用于准确识别陨石星尘的恒星起源,近来,已经从许多前太阳晶粒中提取出独特的硅同位素比。在这里,光离子)融合蒸发反应用于填充核中低旋质子未结合的激发态 决定天体物理速率的 )反应。尤其是, 从共振到 ,现在已确定在217和315 keV处的关键共振为 和 级别。本文提供了217-keV共振强度的第一个估计值,并指出315-keV共振的强度决定了共振频率。)在氧氖新星的整个峰值温度范围内的反应比以前预期的要高。因此,丰富的 在新星爆炸期间喷出的水可能比最新理论模型所预测的要少。