壳模型对13N Gamow-Teller跃迁的研究

支启军; 郑强

doi:10.7498/aps.60.102301

摘要

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.

关键词:

Abstract

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:

作者及机构信息

支启军¹,
郑强²

1.
贵州师范大学物理与电子科学学院,贵阳 550001;

2.
贵州师范大学数学与计算机科学学院,贵阳 550001

基金项目: 国家自然科学基金(批准号:10865004, 11065005,11165006)、贵州省科学技术基金(批准号:[2008]2254)和贵州省国际科技合作基金(批准号:黔科合外G字7026)资助的课题.

Authors and contacts

Zhi Qi-Jun¹,
Zheng Qiang²

1.
School of Physics and Electronic Science, Guizhou Normal University, Guiyang 550001,China;

2.
School of mathematics and computer science, Guizhou Normal University, Guiyang 550001,China

参考文献

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施引文献

[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 55 3197]
[13]
[14]	Zhang J, Wang S F 2010 Acta Phys. Sin. 59 1391 (in Chinese) [张洁、王少峰 2010 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 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 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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