Reaction rate for carbon burning in massive stars

Jiang C. L.; Santiago-Gonzalez D.; Almaraz-Calderon S.; Rehm K. E.; Back B. B.; Auranen K.; Avila M. L.; Ayangeakaa A. D.; Bottoni S.; Carpenter M. P.; Dickerson C.; DiGiovine B.; Greene J. P.; Hoffman C. R.; Janssens R. V. F.; Kay B. P.; Kuvin S. A.; Lauritsen T.; Pardo R. C.; Sethi J.; Seweryniak D.; Talwar R.; Ugalde C.; Zhu S.; Bourgin D.; Courtin S.; Haas F.; Heine M.; Fruet G.; Montanari D.; Jenkins D. G.; Morris L.; Lefebvre-Schuhl A.; Alcorta M.; Fang X.; Tang X. D.; Bucher B.; Deibel C. M.; Marley S. T.

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Reaction rate for carbon burning in massive stars

机译：碳燃烧在大型恒星中的反应速率

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Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C-12 + C-12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C-12 + C-12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around E-cm = 3.5-4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.

机译：碳燃烧是大规模恒星中核酸内酯的关键阶段。点燃该燃烧阶段的条件以及所得灰烬的随后同位素组成，强烈地取决于在非常低的能量下的C-12 + C-12融合的反应速率。该反应的横截面的结果受此类能量测量中遇到的各种背景的影响。在本文中，我们报告了最小化这些背景的C-12 + C-12融合截面的新测量。结果发现，天体物理的因子围绕E-cm = 3.5-4.0 meV显示出最大值，这导致先前预测的天体物理反应速率的降低。

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《Physical review, C》 |2018年第1期|共6页
作者
Jiang C. L.; Santiago-Gonzalez D.; Almaraz-Calderon S.; Rehm K. E.; Back B. B.; Auranen K.; Avila M. L.; Ayangeakaa A. D.; Bottoni S.; Carpenter M. P.; Dickerson C.; DiGiovine B.; Greene J. P.; Hoffman C. R.; Janssens R. V. F.; Kay B. P.; Kuvin S. A.; Lauritsen T.; Pardo R. C.; Sethi J.; Seweryniak D.; Talwar R.; Ugalde C.; Zhu S.; Bourgin D.; Courtin S.; Haas F.; Heine M.; Fruet G.; Montanari D.; Jenkins D. G.; Morris L.; Lefebvre-Schuhl A.; Alcorta M.; Fang X.; Tang X. D.; Bucher B.; Deibel C. M.; Marley S. T.;
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作者单位

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Argonne Natl Lab Phys Div Argonne IL 60439 USA;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ Strasbourg IPHC F-67037 Strasbourg France;

Univ York Dept Phys York YO10 5DD N Yorkshire England;

Univ York Dept Phys York YO10 5DD N Yorkshire England;

CNRS IN2P3 F-91405 Orsay France;

TRIUMF Vancouver BC V6T 2A3 Canada;

Sun Yat Sen Univ Sino French Inst Nucl Engn &

Technol Zhuhai 519082 Peoples R China;

Inst Modern Phys Lanzhou Gansu Peoples R China;

Lawrence Livermore Natl Lab Livermore CA 94551 USA;

Louisiana State Univ Dept Phys &

Astron Baton Rouge LA 70803 USA;

Louisiana State Univ Dept Phys &

Astron Baton Rouge LA 70803 USA;

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中图分类原子核物理学、高能物理学;
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专利

1. Reaction rate for carbon burning in massive stars [J] . Jiang C. L., Santiago-Gonzalez D., Almaraz-Calderon S., Physical review, C . 2018,第1期

机译：碳燃烧在大型恒星中的反应速率
2. ON THE SENSITIVITY OF MASSIVE STAR NUCLEOSYNTHESIS AND EVOLUTION TO SOLAR ABUNDANCES AND TO UNCERTAINTIES IN HELIUM-BURNING REACTION RATES [J] . Clarisse Tur, Alexander Heger, Sam M. Austin The Astrophysical journal . 2007,第1Pt1期

机译：燃烧反应速率中恒星核合成的敏感性以及对太阳丰度和不确定度的演化
3. On the Sensitivity of Massive Star Nucleosynthesis and Evolution to Solar Abundances and to Uncertainties in Helium-Burning Reaction Rates [J] . Clarisse Tur, Alexander Heger, Sam M. Austin The Astrophysical journal . 2007,第1期

机译：大规模恒星核合成和演化对太阳丰度和烧氦反应速率不确定性的敏感性
4. Reaction Rates for H-burning in Stars from Experiments with Radioactive Nuclear Beams [C] . Livius Trache Carpathian School of Physics . 2008

机译：来自放射性核束实验的H型燃烧的反应速率
5. Homogeneous and heterogeneous reaction rates for the reactions of carbon with carbon dioxide and water. [D] . Culbertson, Brad. 2009

机译：碳与二氧化碳和水反应的均相和异相反应速率。
6. Thermal studies of the rates of the reactions of carbon dioxide in concentrated haemoglobin solutions and in red blood cells. A. The reactions catalysed by carbonic anhydrase. B. The carbamino reactions of oxygenated and deoxygenated haemoglobin [O] . J. C. Kernohan, F. J. W. Roughton 1968

机译：对浓缩血红蛋白溶液和红细胞中二氧化碳反应速率的热研究。 A.由碳酸酐酶催化的反应。 B.氧化的和脱氧的血红蛋白的氨基甲酸酯反应
7. Reaction rate for carbon burning in massive stars [O] . Jiang, C.L., Santiago-Gonzalez, D., Almaraz-Calderon, S., 2018

机译：大质量恒星燃烧碳的反应速率

Reaction rate for carbon burning in massive stars

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