论文标题
$^{29} $ si（p，$γ$）$^{30} $ p的热核反应率
Thermonuclear reaction rate of $^{29}$Si(p,$γ$)$^{30}$P
论文作者
论文摘要
$^{29} $ si（p，$γ$）$^{30} $ p反应的热核速率会影响$^{29} $ si的丰富性。可靠的反应速率对于测试前置星星晶粒的Nova亲子关系至关重要。目前，考虑到经典的novae有望是尘土谷物的多产者，在数千种研究中，在原始陨石中没有明确鉴定出古典的Nova谷物。我们研究了$^{29} $ si $+$ $ $ $ p $在质量中心能量的反应$ 200 $ $ - $ 420 $ 〜KEV，目前的共振能量，水平激发能，共振强度，共振强度和分支比率提高了值。在$ 303 $ KEV的质量中心能量中发现了一种新的共鸣。对于预期的共鸣，$ 215 $ 〜KEV，可以确定实验的实验上限。我们评估了质子阈值附近的水平结构，并根据所有可用的实验信息提出了新的反应速率。与以前的结果相比，我们的新反应率降低了，与先前的结果相比，$ t $ $ \ ge $ $ $ 140 $ 〜mk，这对于经典的Nova Nova核合成最为重要。讨论了在较低温度下提高反应速率的未来实验。
The thermonuclear rate of the $^{29}$Si(p,$γ$)$^{30}$P reaction impacts the $^{29}$Si abundance in classical novae. A reliable reaction rate is essential for testing the nova paternity of presolar stardust grains. At present, the fact that no classical nova grains have been unambiguously identified in primitive meteorites among thousands of grains studied is puzzling, considering that classical novae are expected to be prolific producers of dust grains. We investigated the $^{29}$Si $+$ $p$ reaction at center-of-mass energies of $200$ $-$ $420$~keV, and present improved values for resonance energies, level excitation energies, resonance strengths, and branching ratios. One new resonance was found at a center-of-mass energy of $303$ keV. For an expected resonance at $215$~keV, an experimental upper limit could be determined for the strength. We evaluated the level structure near the proton threshold, and present new reaction rates based on all the available experimental information. Our new reaction rates have much reduced uncertainties compared to previous results at temperatures of $T$ $\ge$ $140$~MK, which are most important for classical nova nucleosynthesis. Future experiments to improve the reaction rates at lower temperatures are discussed.
