天体环境下<sup>66</sup>Fe的电子俘获几率计算

秦文韬; 支启军; 杨友昌

doi:10.7498/aps.71.20220929

摘要

弱相互作用几率的计算对于原子核物理和核天体物理具有非常重要的作用. 本文选取在天体环境中非常重要的核素⁶⁶Fe,考虑一级禁戒跃迁, 利用壳模型计算了⁶⁶Fe在不同天体环境下的电子俘获几率, 着重考察了容许Gamow-Teller跃迁和禁戒跃迁的贡献. 结果发现, 在一些天体环境下, 禁戒跃迁对于电子俘获几率有重要贡献, 其中非唯一型禁戒跃迁起主要作用. 我们的结果对于研究原子核弱相互作用和天体环境下的核素合成和演化具有重要作用.

关键词:

Abstract

The calculation of weak interaction rates plays a very important role in studying nuclear physics and nuclear astrophysics. In this work, we calculate the electron capture rate of ⁶⁶Fe in the framework of shell model. We mainly focus on the contribution of allowed transition and forbidden transition to the total rate. It is found that in some astrophysical environments the forbidden transition is very important in contribution to the electron capture rate, in which the non-unique forbidden transition plays a major role. This is very important for nuclear structures and astrophysics.

Keywords:

作者及机构信息

1.
贵州师范大学物理与电子科学学院, 贵阳　550001

2.
贵州师范大学贵州省射电天文数据处理重点实验室, 贵阳　550001

3.
贵州工程应用技术学院, 毕节　551700

4.
遵义师范学院, 遵义　563006

通信作者: 支启军, qjzhi@gznu.edu.cn

基金项目: 国家自然科学基金(批准号:12273008, 11865019, U1731238)、贵州省科学技术基金(批准号: (2016) 4008, [2017]5726-37, [2018]5769-02)和贵州省教育厅(批准号: 黔科合KY字[2020]003号)资助的课题.

Authors and contacts

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

2.
Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing, Guizhou Normal University, Guiyang 550001, China

3.
Guizhou University of Engineering Science, Bijie 551700, China

4.
Zunyi Normal University, Zunyi 563006, China

Corresponding author: Zhi Qi-Jun, qjzhi@gznu.edu.cn

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 12273008, 11865019, U1731238), the Guizhou Provincial Science and Technology Foundation, China (Grant Nos. (2016) 4008, [2017]5726-37, [2018]5769-02), and the Foundation of Education Bureau of Guizhou Province, China (Grant No. KY (2020) 003).

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参考文献

[1]	Bethe H A, Brown G E, Applegate J, Lattimer J M 1979 Nucl. Phys. A 324 487 Google Scholar
[2]	Bethe H A 1990 Rev. Mod. Phys 62 801 Google Scholar
[3]	Fuller G M, Fowler W A, Newman M J 1980 Astrophys. J. Suppl. Ser 42 447 Google Scholar
[4]	Fuller G M, Fowler W A, Newman M J 1982 Astrophys. J. Suppl. Ser 48 279 Google Scholar
[5]	Langanke K, Martinez-Pinedo G 2003 Rev. Mod. Phys. 75 819 Google Scholar
[6]	Janka H T, Langanke K, Marek A, Martinez-Pinedo G, Muller B 2007 Phys. Rep. 442 38 Google Scholar
[7]	Fuller G M, Fowler W A, Newman M J 1982 Astrophys. J. 252 715 Google Scholar
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[22]	Caurier E, Martinez-pinedo G, Nowacki F, Poves A, Zuker A P 2005 Rev. Mod. Phys 77 427 Google Scholar
[23]	张玉美、许甫荣 2008 物理学报 57 4826 Google Scholar Zhang Y M, Xu F R 2008 Acta. Phys. Sin. 57 4826 Google Scholar
[24]	Zhi Q, Caurier E, Cuenca-Garcia J J, Langanke K, Martinez-Pinedo G, Sieja K 2013 Phys. Rev. C 87 025803 Google Scholar
[25]	Toshio S, Takashi Y, Toshitaka K, Takaharu O 2012 Phys. Rev. C 85 015802 Google Scholar
[26]	Sorlin O, Leenhardt S, Donzaud C, Duprat J, Azaiez F, Nowacki F, Grawe H, Dombrádi Z, Amorini F, Astier A, Baiborodin D, Belleguic M, Borcea C, Bourgeois C, Cullen D M, Dlouhy Z, Dragulescu E, Górska M, Grévy S, Guillemaud-Mueller D, Hagemann G, Herskind B, Kiener J, Lemmon R, Lewitowicz M, Lukyanov S M, Mayet P, De Oliveira Santos F, Pantalica D, Penionzhkevich Y E, Pougheon F, Poves A, Redon N, Saint-Laurent M G, Scarpaci J A, Sletten G, Stanoiu M, Tarasov O, Theisen C 2002 Phys. Rev. Lett 88 092501 Google Scholar
[27]	Langanke K, Terasaki J, Nowacki F, Dean D J, Nazarewicz W 2003 Phys. Rev. C 67 044314 Google Scholar
[28]	Honma M, Otsuka T, Brown B A, Mizusaki T 2002 Phys. Rev. C 65 061301 Google Scholar
[29]	Kleis H, Seidlitz M, Blazhev A, Kaya L, Reiter P, Arnswald K, Dewald A, Droste M, Fransen C, Moller O, Shimizu N, Tsunoda Y, Utsuno Y, von Brentano P, Zell K O 2021 Phys. Rev. C 104 034310 Google Scholar
[30]	Hannawald M, Kautzsch T, Wohr A, Walters W B, Kratz K L, Fedoseyev V N, Mishin V I, Bohmer W, Pfeiffer B, Sebastian V, Jading Y, Koster U, Lettry J, Ravn H L 1999 Phys. Rev. Lett. 82 1391 Google Scholar

施引文献

图 1 计算得到的⁶⁶Fe激发态与实验值^[30]的比较

Fig. 1. Comparison of the calculated excited state of ⁶⁶Fe and the experimental value^[30].

下载: 全尺寸图片幻灯片

图 2 ⁶⁶Fe基态的GT与U1 F强度分布　(a) GT强度分布; (b) U1F强度分布

Fig. 2. Strength distributions of GT and U1 F of ⁶⁶Fe ground state: (a) GT strength contributions; (b) U1F strength contributions.

下载: 全尺寸图片幻灯片

图 3 超新星环境下lg(ρYe) = 10.1的⁶⁶Fe电子俘获几率

Fig. 3. ⁶⁶Fe electron captures rates at lg(ρYe) = 10.1 in supernova environment.

下载: 全尺寸图片幻灯片

图 4 超新星环境下lg(ρY_e) = 11.1的⁶⁶Fe电子俘获几率

Fig. 4. ⁶⁶Fe electron captures rates at lg(ρY_e) = 11.1 in supernova environment.

下载: 全尺寸图片幻灯片

图 5 non-U1F跃迁与U1F跃迁在不同温度下贡献的比例

Fig. 5. Ratio of non-u1f transition and u1f transition at different temperatures.

下载: 全尺寸图片幻灯片

图 6 超新星环境下lg(ρY_e) = 10.1的⁶⁶Fe电子俘获几率, 考虑了non-U1F的贡献

Fig. 6. In supernova environment at lg(ρY_e) = 10.1 ⁶⁶Fe electron captures rates which considering the contribution of non-u1f transition

下载: 全尺寸图片幻灯片

[1]	Bethe H A, Brown G E, Applegate J, Lattimer J M 1979 Nucl. Phys. A 324 487 Google Scholar
[2]	Bethe H A 1990 Rev. Mod. Phys 62 801 Google Scholar
[3]	Fuller G M, Fowler W A, Newman M J 1980 Astrophys. J. Suppl. Ser 42 447 Google Scholar
[4]	Fuller G M, Fowler W A, Newman M J 1982 Astrophys. J. Suppl. Ser 48 279 Google Scholar
[5]	Langanke K, Martinez-Pinedo G 2003 Rev. Mod. Phys. 75 819 Google Scholar
[6]	Janka H T, Langanke K, Marek A, Martinez-Pinedo G, Muller B 2007 Phys. Rep. 442 38 Google Scholar
[7]	Fuller G M, Fowler W A, Newman M J 1982 Astrophys. J. 252 715 Google Scholar
[8]	Caurier E, Langanke K, Martínez-Pinedo G, Nowacki F 1999 Nucl. Phys. A 653 439 Google Scholar
[9]	Langanke K, Martínez-Pinedo G 2000 Nucl. Phys. A 673 481 Google Scholar
[10]	张洁, 王少峰 2010 物理学报 59 1391 Google Scholar Zhang J, Wang S F 2010 Acta. Phys. Sin. 59 1391 Google Scholar
[11]	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, Galès 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 Google Scholar
[12]	支启军, 郑强 2011 物理学报 60 102301 Google Scholar Zhi Q, Zheng Q 2011 Acta. Phys. Sin. 60 102301 Google Scholar
[13]	张绍庆, 谢娟, 张小平, 支启军 2016 Acta. Phys. Sin. 65 092101 Google Scholar Zhang S Q, Xie J, Zhang X P, Zhi Q J 2016 物理学报 65 092101 Google Scholar
[14]	You J L, Wu Q D, Zhang X P, Zhi Q 2019 Commun. Theor. Phys 71 293 Google Scholar
[15]	You J L, Zhang X P, Zhi Q J, Ren Z Z, Wu Q D 2019 Chin. Phys. C 43 114104 Google Scholar
[16]	Mukai M, Hirayama Y, Watanabe Y X, Watanabe H, Koura H, Jeong S C, Miyatake H, Brunet M, Ishizawa S, Kondev F G, Lane G J, Litvinov Y A, Niwase T, Oyaizu M, Podolyak Z, Rosenbusch M, Schury P, Wada M, Walker P M 2022 Phys. Rev. C 105 034331 Google Scholar
[17]	Zhi Q, Langanke K, Martinez-Pinedo G, Nowacki F, Sieja K 2011 Nucl. Phys. A 859 172 Google Scholar
[18]	Stryjczyk M, Tsunoda Y, Darby I G, Witte H D, Diriken J, Fedorov D V, Fedosseev V N, Fraile L M, Huyse M, Köster U, Marsh B A, Otsuka T, Pauwels D, Popescu L, Radulov D, Seliverstov M D, Sjödin A M, P. Van den Bergh, Van Duppen P, Venhart M, Walters W B, Wimmer K 2018 Phys. Rev. C 98 064326 Google Scholar
[19]	Qi C and Xu F. R 2008 Nucl. Phys. A 800 47 Google Scholar
[20]	Qi C and Xu F. R 2008 Nucl. Phys. A 814 48 Google Scholar
[21]	支启军 2011 物理学报 60 052101 Google Scholar Zhi Q J 2011 Acta. Phys. Sin. 60 052101 Google Scholar
[22]	Caurier E, Martinez-pinedo G, Nowacki F, Poves A, Zuker A P 2005 Rev. Mod. Phys 77 427 Google Scholar
[23]	张玉美、许甫荣 2008 物理学报 57 4826 Google Scholar Zhang Y M, Xu F R 2008 Acta. Phys. Sin. 57 4826 Google Scholar
[24]	Zhi Q, Caurier E, Cuenca-Garcia J J, Langanke K, Martinez-Pinedo G, Sieja K 2013 Phys. Rev. C 87 025803 Google Scholar
[25]	Toshio S, Takashi Y, Toshitaka K, Takaharu O 2012 Phys. Rev. C 85 015802 Google Scholar
[26]	Sorlin O, Leenhardt S, Donzaud C, Duprat J, Azaiez F, Nowacki F, Grawe H, Dombrádi Z, Amorini F, Astier A, Baiborodin D, Belleguic M, Borcea C, Bourgeois C, Cullen D M, Dlouhy Z, Dragulescu E, Górska M, Grévy S, Guillemaud-Mueller D, Hagemann G, Herskind B, Kiener J, Lemmon R, Lewitowicz M, Lukyanov S M, Mayet P, De Oliveira Santos F, Pantalica D, Penionzhkevich Y E, Pougheon F, Poves A, Redon N, Saint-Laurent M G, Scarpaci J A, Sletten G, Stanoiu M, Tarasov O, Theisen C 2002 Phys. Rev. Lett 88 092501 Google Scholar
[27]	Langanke K, Terasaki J, Nowacki F, Dean D J, Nazarewicz W 2003 Phys. Rev. C 67 044314 Google Scholar
[28]	Honma M, Otsuka T, Brown B A, Mizusaki T 2002 Phys. Rev. C 65 061301 Google Scholar
[29]	Kleis H, Seidlitz M, Blazhev A, Kaya L, Reiter P, Arnswald K, Dewald A, Droste M, Fransen C, Moller O, Shimizu N, Tsunoda Y, Utsuno Y, von Brentano P, Zell K O 2021 Phys. Rev. C 104 034310 Google Scholar
[30]	Hannawald M, Kautzsch T, Wohr A, Walters W B, Kratz K L, Fedoseyev V N, Mishin V I, Bohmer W, Pfeiffer B, Sebastian V, Jading Y, Koster U, Lettry J, Ravn H L 1999 Phys. Rev. Lett. 82 1391 Google Scholar

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天体环境下⁶⁶Fe的电子俘获几率计算