Impact factor of Chinese Physics C is 3.6 in 2023 Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
Advanced Search
×
近期发现有不法分子冒充我刊与作者联系，借此进行欺诈等不法行为，请广大作者加以鉴别，如遇诈骗行为，请第一时间与我刊编辑部联系确认（《中国物理C》（英文）编辑部电话：010-88235947,010-88236950），并作报警处理。
本刊再次郑重声明：
（1）本刊官方网址为cpc.ihep.ac.cn和https://iopscience.iop.org/journal/1674-1137
（2）本刊采编系统作者中心是投稿的唯一路径，该系统为ScholarOne远程稿件采编系统，仅在本刊投稿网网址（https://mc03.manuscriptcentral.com/cpc）设有登录入口。本刊不接受其他方式的投稿，如打印稿投稿、E-mail信箱投稿等，若以此种方式接收投稿均为假冒。
（3）所有投稿均需经过严格的同行评议、编辑加工后方可发表，本刊不存在所谓的“编辑部内部征稿”。如果有人以“编辑部内部人员”名义帮助作者发稿，并收取发表费用，均为假冒。
                  
《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2017, Vol. 41> Issue(9) : 095101 DOI: 10.1088/1674-1137/41/9/095101

Strongly screening electron capture for nuclides 52, 53, 59, 60Fe by the Shell-Model Monte Carlo method in pre-supernovae

  • 1.

      College of Marine Science and Technology, Hainan Tropical Ocean University, Sanya 572022, China

  • 2.

      Department of Astronomy, Nanjing University, Nanjing, Jiangshu 210000, China

  • The death of massive stars due to supernova explosions is a key ingredient in stellar evolution and stellar population synthesis. Electron capture (EC) plays a vital role in supernova explosions. Using the Shell-Model Monte Carlo method, based on the nuclear random phase approximation and linear response theory model for electrons, we study the strong screening EC rates of 52, 53, 59, 60Fe in pre-supernovae. The results show that the screening rates can decrease by about 18.66%. Our results may become a good foundation for future investigation of the evolution of late-type stars, supernova explosion mechanisms and numerical simulations.
      PCAS:
  • 加载中

  • References

    [1] J. J. Liuand W. M. Gu, ApJS., 224:29(2016)
    [2] J. J. Liu, MNRAS., 438:930(2014)
    [3] J. J. Liu and D. M. Liu., ApSS., 361:246(2016)
    [4] G. M. Fuller, W. A. Fowler, and M. J. Newman, ApJ., 42:447(1980)
    [5] G. M. Fuller, W. A. Fowler, and M. J. Newman, ApJS., 48:279(1982)
    [6] M. B. Aufderheide, G. E. Brown, T. T. S. kuo, D. B. Stout, and P. Vogel., ApJ., 362:241(1990)
    [7] M. B. Aufderheide, I. Fushikii, S. E. Woosely, and D. H. Hartmanm, ApJS., 91:389(1994)
    [8] M. H. Johnson and B. A. Lippmann, PhRv., 76:828(1949)
    [9] W. E. Ormand, D. J. Dean, C. W. Johnson, et al., PhRvC., 49:1422(1994)
    [10] S. E. Koonin, D. J. Dean, and K., Langanke, PhRep., 278:1(1997)
    [11] Y. Alhassid, D. J. Dean, S. E. Koonin et al, PhRvL.,72:613(1994)
    [12] K. Langanke and G. Martinez-Pinedo, Phys. Lett. B., 436:19(1998)
    [13] K. Langanke and G. Martinez-Pinedo, Nuclear Phys. A., 673:481(2000)
    [14] A. Juodagalvis, K. Langanke, W. R. Hix et al, Nuclear Phys. A., 848:454(2010)
    [15] Z. F. Gao, N. Wang, J. P. Yuan, L. Jiang, and D. L. Song, ApSS., 332:129(2011)
    [16] J. J. Liu and Z. Q. Luo, Chin. Phys. Lett., 16:1861(2007)
    [17] J. J. Liu and Z. Q. Luo, Chin. Phys., 16:2671(2007)
    [18] J. J. Liu and Z. Q. Luo, Chin. Phys., 16:3624(2007)
    [19] J. J. Liu and Z. Q. Luo, Chin.Phys. C, 32:108(2008)
    [20] J. J. Liu and Z. Q. Luo, Comm.Theo. Phys., 49:239(2008)
    [21] J. J. Liu, X. P. Kang et al, Chin. Phys. C, 35:243(2011)
    [22] J. J. Liu, Chin. Phys. C, 34:171(2010)
    [23] J. J. Liu, Chin. Phys. C, 34:190(2010)
    [24] J. J. Liu, Q. H, Peng, L. H. Hao et al, RAA., arXiv:1707.03504(2017)
    [25] J. J. Liu, Chin. Phys. C, 37:51018(2013)
    [26] J. Nabi and H. V. Klapdor-Kleingrothaus, EPJA, 337:339(1999)
    [27] D. J. Dean, K. Langanke, L. Chatterjee, P. B. Radha, and M. R. Strayer, Phys. Rev. C, 58:536(1998)
    [28] A. Heger, S. E. Woosley, G. Martinez-Pinedo, and K. Langanke, ApJ., 560:307(2001)
    [29] J. Gutierrez, E. Garcia-Berro, I. Iben et al, ApJ., 459:701(1996)
    [30] E. Bravo and D. Garcia-Senz, MNRAS., 307:984(1999)
    [31] J. J. Liu, Chin. Phys. B, 19:099601(2010)
    [32] N. Itoh, N. Tomizawa, M. Tamamura et al, ApJ., 579:380(2002)
    [33] Z. Q. Luo and Q. H. Peng, ChAA, 25:1(2001)
    [34] K. Langanke, E. Kolbe, and D.J. Dean, Phys. Rev. C, 63:032801(2001)
    [35] D.R. Bes and R.A. Sorensen, Adv. Nucl. Phys., 2:129(1969)
    [36] E. Kolbe, K. Langanke, and P. Vogel, Nucl. Phys. A., 652:91(1999)
    [37] J. Cooperstein, and J. Wambach, Nuclear Phys. A, 420:591(1984)
    [38] M. W. C.Dharma-wardana, and F. Perrot, Phys. Rev. A, 26:2096(1982)
    [39] D. Pines and P. Nozie'res, The Theory of Quantum Liquids (New York:W. A. Benjamin, 1966)
    [40] B. Jancovici, Nuovo Cimento, 25:428(1962)
    [41] P. A. Seeger and W. M. Howard, Nucl. Phys. A, 238:491(1975)

  • Access

    加载中

Get Citation
Jing-Jing Liu, Qiu-He Peng and Dong-Mei Liu. Strongly screening electron capture for nuclides 52, 53, 59, 60Fe by the Shell-Model Monte Carlo method in pre-supernovae[J]. Chinese Physics C, 2017, 41(9): 095101. doi: 10.1088/1674-1137/41/9/095101
Jing-Jing Liu, Qiu-He Peng and Dong-Mei Liu. Strongly screening electron capture for nuclides 52, 53, 59, 60Fe by the Shell-Model Monte Carlo method in pre-supernovae[J]. Chinese Physics C, 2017, 41(9): 095101.  doi: 10.1088/1674-1137/41/9/095101 shu
Milestone
Received: 2017-02-13
Revised: 2017-04-24
Fund

    Supported by National Natural Science Foundation of China (11565020), Counterpart Foundation of Sanya (2016PT43), Special Foundation of Science and Technology Cooperation for Advanced Academy and Regional of Sanya (2016YD28), Scientific Research Staring Foundation for 515 Talented Project of Hainan Tropical Ocean University (RHDRC201701) and Natural Science Foundation of Hainan Province (114012)

Article Metric

Article Views(1826)
PDF Downloads(36)
Cited by(0)
Policy on re-use
To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.
通讯作者: 陈斌, bchen63@163.com
  • 1. 

    沈阳化工大学材料科学与工程学院 沈阳 110142

  1. 本站搜索
  2. 百度学术搜索
  3. 万方数据库搜索
  4. CNKI搜索

Email This Article

Title:
Email:

Strongly screening electron capture for nuclides 52, 53, 59, 60Fe by the Shell-Model Monte Carlo method in pre-supernovae

    Corresponding author: Jing-Jing Liu,
    Corresponding author: Dong-Mei Liu,
  • 1.  College of Marine Science and Technology, Hainan Tropical Ocean University, Sanya 572022, China
  • 2.  Department of Astronomy, Nanjing University, Nanjing, Jiangshu 210000, China
  • Received Date: 2017-02-13
  • Accepted Date: 2017-04-24
  • Available Online: 2017-09-05
Fund Project:  Supported by National Natural Science Foundation of China (11565020), Counterpart Foundation of Sanya (2016PT43), Special Foundation of Science and Technology Cooperation for Advanced Academy and Regional of Sanya (2016YD28), Scientific Research Staring Foundation for 515 Talented Project of Hainan Tropical Ocean University (RHDRC201701) and Natural Science Foundation of Hainan Province (114012)

Abstract: The death of massive stars due to supernova explosions is a key ingredient in stellar evolution and stellar population synthesis. Electron capture (EC) plays a vital role in supernova explosions. Using the Shell-Model Monte Carlo method, based on the nuclear random phase approximation and linear response theory model for electrons, we study the strong screening EC rates of 52, 53, 59, 60Fe in pre-supernovae. The results show that the screening rates can decrease by about 18.66%. Our results may become a good foundation for future investigation of the evolution of late-type stars, supernova explosion mechanisms and numerical simulations.

    HTML

Reference (41)

目录

Link
IOPScience
SCOAP3
arXiv
Chinese Physical Society
Journal information
Introduction
Editorial Board
Others
Subscribe
Contact us
QQ: 1307685413
Tel: +86-010-88235947
Fax: +86-010-88233126
E-mail: cpc@ihep.ac.cn

  • CPC Website

  • IOP Website

  • CPC WeChat

Copyright © Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049, China 京ICP备05002789号-1

Supported by: Beijing Renhe Information Technology Co. Ltd  E-mail: info@rhhz.net

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return