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最近的研究表明13N的beta衰变对于Ia型超新星爆炸前的电子丰度有着重要的影响.本文在壳模型的基础上,首先计算13N基态到基态以及基态到不同激发态的Gamow-Teller(GT)跃迁强度,并将其与实验数据进行了比较.在理论计算的GT强度基础上,对不同温度和密度天体环境下13N的电子俘获率进行了细致的计算,并重点讨论基态到激发态的GT跃迁对电子俘获率变化的影响.结果表明,考虑基态到激发态的跃迁后,超新星的电子丰度下降,中微子能量损失增大.基态到激发态跃迁对电子俘获率的影响主要由低激发能级贡献.
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关键词:
- Gamow-Teller跃迁 /
- 壳模型 /
- 电子俘获 /
- 激发态
Recent researches show that the beta decay of 13N can affect the electron abundance before the collapse of SNe Ia supernovae. Based on the shell model, the Gamow-Teller transition strengths from ground state to ground state and trom ground state to excited state of 13N are calculated and the results are compared with theoretical results and also with experimental data. The electron capture rates at different temperatures and densities are calculated and the effect of ground state on excited state transition is discussed. It is shown that due to the transition from ground state to excited state, the electron abundance of the SNe Ia supernovae decreases and the contributions are determined mainly by the low-lying excited states.-
Keywords:
- gamow-teller transition /
- shell model /
- electron capture /
- excited states
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[1] Bethe H A, Brown G E, Applegate J, Lattimer J M 1979 Nucl. Phys. A 324 487
[2] Fuller G M, Fowler W A, Newman M J 1980 Astr. Phys. Jour. Supp. 42 447
[3] [4] Fuller G M, Fowler W A, Newman M J 1982 Astr. Phys. Jour. Supp. 48 279
[5] [6] [7] Langanke K, Martinez-Pinedo 2003 Rev. Mod. Phys 75 819
[8] [9] Langanke K, Martnez-Pinedo G 2000 Nucl. Phys. A 673 481
[10] [11] Nabi J U, Klapdor-Kleingrothaus H V 2004 At. Data Nucl. Data Tables. 88 237
[12] Liu M Q, Zhang J, Luo Z Q 2006 Acta Phys. Sin. 55 3197 (in Chinese) [刘门全、张 洁、罗志全 2006 物理学报 55 3197]
[13] [14] Zhang J, Wang S F 2010 Acta Phys. Sin. 59 1391 (in Chinese) [张 洁、王少峰 2010 物理学报 59 1391]
[15] [16] Zegers R G T, Brown E F, Akimune H, Austin S M, Vanden Berg A M, Brown B A, Chamulak D A, Fujita Y, Fujiwara M, Gals S, Harakeh M N, Hashimoto H, Hayami R, Hitt G W, Itoh M, Kawabata T, Kawase K, Kinoshita M, Nakanishi K, Nakayama S, Okumura S, Shimbara Y, Uchida M, Ueno H, Yamagata T, Yosoi M 2008 Phys. Rev. C 77 024307
[17] [18] [19] Chamulak D A, Brown E F, Timmes F X, Dupczak K 2008 Astr. Phys. Jour. 677 160
[20] [21] Gupta S S, Kawan o T, Mller P 2008 Phys. Rev. Lett. 101,231101
[22] [23] Caurier E, Martinez-pinedo G, Nowacki F, Poves A, Zuker A 2005 Rev. Mod. Phys. 799 427
[24] [25] Qi C, Xu F R 2008 Nucl. Phys. A 800 47
[26] Qi C, Xu F R 2008 Nucl. Phys. A 814 48
[27] [28] Zhi Q J 2011 Acta Phys. Sin. 60 05210(in Chinese)[支启军 2011 物理学报 60 05210]
[29] [30] [31] Zhang Y M, Xu F R 2008 Acta Phys. Sin. 57 4826 (in Chinese) [张玉美、许甫荣 2008 物理学报 57 4826]
[32] [33] Cohen S, Kurath D 1967 Nucl. Phys. A 101 1
[34] [35] Wang X, Rapaport J, Palarczyk M, Hautala C, Yang X, Prout D L, Heerden I V, Howes R, Parks S, Sugarbaker E, Brown B A 2001 Phys. Rev. C 63 024608
[36] Taddeucci T N, Goulding C A, Carey R C 1987 Nucl. Phys. A 469 125
[37] [38] [39] Luo Z Q, Liu H L , Liu J J, Lai X J 2009 Chin. Phys. B 18 377
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