Calculations of electron capture rates of <sup>66</sup>Fe in astrophysical enviroment

Qing Wen-Tao; Zhi Qi-Jun; Yang You-Chang

doi:10.7498/aps.71.20220929

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:

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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References

[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
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[24]	Zhi Q, Caurier E, Cuenca-Garcia J J, Langanke K, Martinez-Pinedo G, Sieja K 2013 Phys. Rev. C 87 025803 Google Scholar
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[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
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Cited By

图 1 计算得到的⁶⁶Fe激发态与实验值^[30]的比较

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

DownLoad: Full-Size Img PowerPoint

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

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

DownLoad: Full-Size Img PowerPoint

图 3 超新星环境下lg(ρYe) = 10.1的⁶⁶Fe电子俘获几率

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

DownLoad: Full-Size Img PowerPoint

图 4 超新星环境下lg(ρY_e) = 11.1的⁶⁶Fe电子俘获几率

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

DownLoad: Full-Size Img PowerPoint

图 5 non-U1F跃迁与U1F跃迁在不同温度下贡献的比例

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

DownLoad: Full-Size Img PowerPoint

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

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

DownLoad: Full-Size Img PowerPoint

[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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Calculations of electron capture rates of ⁶⁶Fe in astrophysical enviroment

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

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Calculations of electron capture rates of 66Fe in astrophysical enviroment

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Authors and contacts

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

FullText HTML : translate this paragraph

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Calculations of electron capture rates of ⁶⁶Fe in astrophysical enviroment