Chapter IV. Nucleon Superfluidity under Pion Condensation in Neutron Star Matter

1993 ◽  
Vol 112 ◽  
pp. 107-122 ◽  
Author(s):  
Tatsuyuki Takatsuka ◽  
Ryozo Tamagaki
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Pion Condensation ◽  
Nucleon Superfluidity

scholarly journals Pion Condensation in Neutron Star Matter

1976 ◽  
Vol 55 (5) ◽  
pp. 1477-1487 ◽  
Author(s):  
A. Suzuki
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Pion Condensation

scholarly journals Instability of Neutron Star Matter for Pion Condensation

1975 ◽  
Vol 54 (5) ◽  
pp. 1429-1439 ◽  
Author(s):  
A. Suzuki ◽  
Y. Futami ◽  
Y. Takahashi
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Pion Condensation

Criteria for pion condensation thresholds in neutron star matter

1974 ◽  
Vol 51 (1) ◽  
pp. 1-4 ◽  
Author(s):  
C.-K. Au ◽  
G. Baym ◽  
E. Flowers
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Pion Condensation

Effects of tensor couplings of ω and ρ mesons on 1S0 nucleon superfluidity in neutron star matter

2016 ◽  
Vol 25 (05) ◽  
pp. 1650059 ◽  
Author(s):  
Xiu-Lin Huang ◽  
Yan Xu ◽  
Cheng-Zhi Liu ◽  
Guang-Zhou Liu
Keyword(s):  
Neutron Star ◽  
Density Range ◽  
Neutron Star Matter ◽  
Hartree Fock ◽  
Relativistic Formula ◽  
Text Model ◽  
Nucleon Superfluidity

The [Formula: see text] nucleon superfluidity in neutron star matter was investigated in the framework of relativistic [Formula: see text] model with the tensor couplings of [Formula: see text] and [Formula: see text] mesons using the relativistic Hartree–Fock (RHF) approximation. It was found that the tensor couplings of [Formula: see text] and [Formula: see text] mesons lead to a clear growth of the [Formula: see text] neutron pairing gap in the density range where there exists [Formula: see text] neutron superfluidity. The [Formula: see text] pairing gap of proton with the tensor couplings of [Formula: see text] and [Formula: see text] mesons in the density range of [Formula: see text]–[Formula: see text][Formula: see text]fm[Formula: see text] is lower and then in the density range of [Formula: see text]–[Formula: see text][Formula: see text]fm[Formula: see text] higher than the corresponding value without the tensor couplings of [Formula: see text] and [Formula: see text] mesons. Our results provide a basic to understand the influence of the tensor couplings of [Formula: see text] and [Formula: see text] mesons on the cooling properties of neutron star.

1 S 0 Nucleon Superfluidity in Neutron Star Matter

2013 ◽  
Vol 30 (6) ◽  
pp. 062101 ◽  
Author(s):  
Yan Xu ◽  
Guang-Zhou Liu ◽  
Cheng-Zhi Liu ◽  
Cun-Bo Fan ◽  
Xing-Wei Han ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutron Star Matter ◽  
Nucleon Superfluidity
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