Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
Advanced Search
Chinese Physics C> 2003, Vol. 27> Issue(12) : 1084-1088 

Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter

  •  Institute of Modern Physics,CAS,Lanzhou 730000,China

  • The proton and neutron 1S0 pairing gaps in β-stable neutron star matter have been studied by using the isospin dependent Brueckner-Hartree-Fock approach and the BCS theory. We have concentrated on investigating and discussing the effect of three-body force. The calculated results indicate that the three-body force has only a small effect on the neutron 1S0 superfluidity in β-stable neutron matter, i.e., it leads to a small reduction of the neutron 1S 0 paring gap. However the three-body force not only suppresses strongly the strength of the proton1S0 superfluidity in β-stable neutron star matter but also reduces largely the density domain for the proton 1S0 superfluidity phase from ρ B<0.45fm－3 to ρB<0.3fm－3. It is also shown that the three-body force enhances largely the proton fraction in β-stable neutron star matter at high densities.
  • 加载中

  • References

    [1] . Migdal A B et al.Sov.Phys.JETP ,1960,10:1762. Pethick C J et al.Annu.Rev.Nucl.Part.Sci.,1995,45:4293. Pines D ,Alpar M A .Nature,1985,316:274. Shapiro S L ,Teukolsky S A .Black Holes,White Dwrfs and Neutron Stars,New York:John Wiley,19835. Baldo M ,Cugnon J ,Lejeune A et al.Nucl.Phys.,1992,A536:3496. Elgaroy O et al.Phys.Rev.Lett.,1996,77:14287. ZUO Wei et al.High Energy Phys.and Nucl.Phys.,2002,26:1134(in Chinese)(左维等.高能物理与核物理,2002,26:1134)8. Migdal A B .Theory of Finite Fermi Systems and Applications to Atomic Nuclei,London:Interscience Publisher,19679. Ring P ,Schuck P .The Nuclear Many-body Problem,New York:Springer-Verlag,198010. Baldo M ,Cugnon J,Lejeune A et al.Nucl.Phys.,1990,A515:40911. Lombardo U ,Schulze H J .Lecture Notes in Physics,2001,578:3012. Clark J W ,Kallman C G ,Yang C H et al.Phys.Lett.,1976,B61:33113. Ainsworth T L ,Wambach J ,Pines D .Phys.Lett.,1989,B222:17314. Schulze H J,Cugnon J ,Lejeune A et al.Phys.Lett.,1996,B375:115. Day B D .Rev.Mod.Phys.,1967,39:719;Jeukenne J P et al.Phys.Rep.,1976,25:83;ZUO Wei et al.High Energy Phys.and Nucl.Phys.,2002,26:703(in Chinese)(左维等.高能物理与核物理,2002,26:703) 16. Wiringa R B ,Stoks V G J,Schiavilla R .Phys.Rev.,1995,C51:2817. Grange P et al.Phys.Rev.,1989,C40:1040 18. SONG H Q et al.Phys.Rev.Lett.,1998,81:158419. Lattimer J M ,Pethick C J,Prakash M et al.Phys.Rev.Lett.,1991,66:2701;Pethick C J.Rev.Mod.Phys.,1992,64:113320. ZUO Wei et al.HEPNP ,2002,26:1238(in Chinese)(左维等.高能物理与核物理,2002,26:1238)21. Machleidt R .Adv.Nucl.Phys.,1989,16:18922. ZUO Wei et al.Phys.Rev.,2002,C66:03730323. Bombaci I ,Lombardo U .Phys.Rev.,1991,C44:1892

  • Access

    加载中

Get Citation
LI Zeng-Hua, LU Guang-Cheng and ZUO Wei. Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(12): 1084-1088.
LI Zeng-Hua, LU Guang-Cheng and ZUO Wei. Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(12): 1084-1088. shu
Milestone
Received: 2003-02-26
Revised: 1900-01-01
Article Metric

Article Views(1144)
PDF Downloads(710)
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:

Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron 1S0 Superfluidity in Neutron Star Matter

    Corresponding author: ZUO Wei,
  • Institute of Modern Physics,CAS,Lanzhou 730000,China
  • Received Date: 2003-02-26
  • Accepted Date: 1900-01-01
  • Available Online: 2003-12-05

Abstract: The proton and neutron 1S0 pairing gaps in β-stable neutron star matter have been studied by using the isospin dependent Brueckner-Hartree-Fock approach and the BCS theory. We have concentrated on investigating and discussing the effect of three-body force. The calculated results indicate that the three-body force has only a small effect on the neutron 1S0 superfluidity in β-stable neutron matter, i.e., it leads to a small reduction of the neutron 1S 0 paring gap. However the three-body force not only suppresses strongly the strength of the proton1S0 superfluidity in β-stable neutron star matter but also reduces largely the density domain for the proton 1S0 superfluidity phase from ρ B<0.45fm－3 to ρB<0.3fm－3. It is also shown that the three-body force enhances largely the proton fraction in β-stable neutron star matter at high densities.

    HTML

Reference (1)

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