The effects of thermonuclear reaction-rate variations on nova nucleosynthesis:: A sensitivity study
The effects of thermonuclear reaction-rate variations on nova nucleosynthesis:: A sensitivity study
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DOI：
10.1086/341400
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发表时间：
2002-09-01
影响因子：
8.7
通讯作者：
Tupper, P
中科院分区：
文献类型：
--
作者：
Iliadis, C;Champagne, A;Tupper, P
我们研究了热核反应速率不确定性对新星核合成的影响。通过采用最热氢燃烧区域（即发生大部分核合成的区域）的温度-密度-时间曲线来进行单区域核合成计算。我们从最近发表的七个不同的流体动力学新星模拟中获得了我们的剖面图，涵盖了 T 峰值 = 0.145 至 0.418 GK 范围内的峰值温度。对于每个剖面，我们在相关误差范围内分别改变了 175 个反应的速率，并分析了质量范围低于 A = 40 的 142 个同位素的丰度变化。总共，我们进行了大约 7350 个核反应网络计算。我们使用质量范围 A = 1-20 和 20-10 的最新热核反应速率评估。对于理论天体物理学家来说，我们的结果表明新星核合成计算在多大程度上依赖于当前不确定的核物理输入，而对于实验核物理学家来说，我们的结果至少代表了稳定和放射性离子束设施未来测量的定性指南。我们发现目前的反应速率估计对于新星核合成中 Li、Be、C 和 N 丰度的预测是可靠的。然而，为了预测更可靠的 O、F、Ne、Na、Mg、Al、Si、S、Cl 和 Ar 丰度，必须显着降低几个反应的速率不确定性。每个采用的新星模拟的结果以表格形式呈现。
We investigate the effects of thermonuclear reaction-rate uncertainties on nova nucleosynthesis. One-zone nucleosynthesis calculations have been performed by adopting temperature-density-time profiles of the hottest hydrogen-burning zone (i.e., the region in which most of the nucleosynthesis takes place). We obtain our profiles from seven different, recently published, hydrodynamic nova simulations covering peak temperatures in the range from T-peak = 0.145 to 0.418 GK. For each of these profiles, we individually varied the rates of 175 reactions within their associated errors and analyzed the resulting abundance changes of 142 isotopes in the mass range below A = 40. In total, we performed approximate to7350 nuclear reaction network calculations. We use the most recent thermonuclear reaction-rate evaluations for the mass ranges A = 1-20 and 20-10. For the theoretical astrophysicist, our results indicate the extent to which nova nucleosynthesis calculations depend on currently uncertain nuclear physics input, while for the experimental nuclear physicist, our results represent at least a qualitative guide for future measurements at stable and radioactive ion beam facilities. We find that present reaction-rate estimates are reliable for predictions of Li, Be, C, and N abundances in nova nucleosynthesis. However, rate uncertainties of several reactions have to be reduced significantly in order to predict more reliable O, F, Ne, Na, Mg, Al, Si, S, Cl, and Ar abundances. Results are presented in tabular form for each adopted nova simulation.