The equations ofstate of the neutron star matter are calculated in the relativistic mean-field approximation witl different hyperon coupling constants. The properties of neutron stars are studied by solving the Oppenh...The equations ofstate of the neutron star matter are calculated in the relativistic mean-field approximation witl different hyperon coupling constants. The properties of neutron stars are studied by solving the OppenheimerVolkoff equation. It manifests the properties of neutron stars - change explicitly as different hyperon coupling constants are concerned.展开更多
By using the new experimental data of AA potential, this paper has performed a full calculation for strange hadronic matter with different strangeness contents as well as its consequences on the global properties of n...By using the new experimental data of AA potential, this paper has performed a full calculation for strange hadronic matter with different strangeness contents as well as its consequences on the global properties of neutron star matter in relativistic mean field model. It finds that the new weak hyperon-hyperon interaction makes the equations of state much stiffer than the result of the previous strong hyperon hyperon interaction, and even stiffer than the result without consideration of hyperon-hyperon interaction. This new hyperon-hyperon interaction results in a maximum mass of 1.75M⊙ （where M⊙ stands for the mass of the Sun）, about 0.2-0.5M⊙ larger than the previous prediction with the presence of hyperons. After examining carefully the onset densities of kaon condensation it finds that this new weak version of hyperon-hyperon interaction favours the occurrence of kaons in comparison with the strong one.展开更多
In the framework of the relativistic mean field theory including the hyperon-hyperon(YY) interactions,protoneutron stars with a weakly interacting light U boson are studied. The U-boson leads to the increase of the st...In the framework of the relativistic mean field theory including the hyperon-hyperon(YY) interactions,protoneutron stars with a weakly interacting light U boson are studied. The U-boson leads to the increase of the star maximum mass. The modification to the maximum mass by the U-boson with the strong YY interaction is larger than that with the weak YY interaction. The maximum mass of the protoneutron star is less sensitive to the U-boson than that of the neutron star. The inclusion of the U-boson narrows down the mass window for the hyperonized protoneutron stars. As g^2/μ~2 increases, the species of hyperons, which can appear in a stable protoneutron star decrease. The rotation frequency, the red shift, the momentum of inertia and the total neutrino fraction of PSR J1903-0327 are sensitive to the U-boson and change with g^2/μ~2 in an approximate linear trend. The possible way to constrain the coupling constants of the U-boson is discussed.展开更多
The difference between the transition density of a larger mass hyperon star （for example, the neutron star PSR J1614-2230） and that of a smaller mass hyperon star is investigated in the framework of the relativistic...The difference between the transition density of a larger mass hyperon star （for example, the neutron star PSR J1614-2230） and that of a smaller mass hyperon star is investigated in the framework of the relativistic mean field theory. We see that the transition density p0H increases with the increase of xw （i.e. the mass of the neutron star）. For the nucleons parts, the neutrons make the main contribution to the transition density as the baryon density P=p0H. With the increase of the xw （i.e. the mass of the neutron star）, the relative particle number density of neutrons decreases while that of protons increases. For the parts of hyperons, the ∧ and ≡. make the main contributions to the transition density as the baryon density p=p0H. The relative particle number density of A decreases while that of ≡ increases with the increase of the xw （i.e. the mass of the neutron star）. For the hyperons ∑-, ∑0 and E-, the total contributions are less than 16 per cent.展开更多
文摘The equations ofstate of the neutron star matter are calculated in the relativistic mean-field approximation witl different hyperon coupling constants. The properties of neutron stars are studied by solving the OppenheimerVolkoff equation. It manifests the properties of neutron stars - change explicitly as different hyperon coupling constants are concerned.
基金Project supported by the National Natural Science Foundation of China （Grant Nos 10575119 and 10235030）, the Knowledge Innovation Project （Grant No KJCX2-SW-N02） of Chinese Academy of Sciences, the Major State Basic Research Development Program of China （Grant No G2000077400）, the Major Prophase Research Project of Fundamental Research of the Ministry of Science and Technology of China （Grant No 2002CCB00200）, and the Asia Europe Link project （Grant No CN/ASIA-LINK/008（94791）） of the European Commission.
文摘By using the new experimental data of AA potential, this paper has performed a full calculation for strange hadronic matter with different strangeness contents as well as its consequences on the global properties of neutron star matter in relativistic mean field model. It finds that the new weak hyperon-hyperon interaction makes the equations of state much stiffer than the result of the previous strong hyperon hyperon interaction, and even stiffer than the result without consideration of hyperon-hyperon interaction. This new hyperon-hyperon interaction results in a maximum mass of 1.75M⊙ （where M⊙ stands for the mass of the Sun）, about 0.2-0.5M⊙ larger than the previous prediction with the presence of hyperons. After examining carefully the onset densities of kaon condensation it finds that this new weak version of hyperon-hyperon interaction favours the occurrence of kaons in comparison with the strong one.
基金Supported by Jiangsu Province Natural Science Foundation Youth Fund of China under Grant No.Bk20140982National Natural Science Foundation of China under Grant No.11447165+1 种基金Youth Innovation Promotion Association,Chinese Academy of Sciences under Grant No.2016056the Development Project of Science and Technology of Jilin Province under Grant No.20180520077JH
文摘In the framework of the relativistic mean field theory including the hyperon-hyperon(YY) interactions,protoneutron stars with a weakly interacting light U boson are studied. The U-boson leads to the increase of the star maximum mass. The modification to the maximum mass by the U-boson with the strong YY interaction is larger than that with the weak YY interaction. The maximum mass of the protoneutron star is less sensitive to the U-boson than that of the neutron star. The inclusion of the U-boson narrows down the mass window for the hyperonized protoneutron stars. As g^2/μ~2 increases, the species of hyperons, which can appear in a stable protoneutron star decrease. The rotation frequency, the red shift, the momentum of inertia and the total neutrino fraction of PSR J1903-0327 are sensitive to the U-boson and change with g^2/μ~2 in an approximate linear trend. The possible way to constrain the coupling constants of the U-boson is discussed.
基金Supported by Anhui Provincial Natural Science Foundation(1208085MA09)Scientific Research Program Foundation of the Higher Education Institutions of Anhui Province"Study on the Massive Neutron Star PSR J0348+0432 in the Framework of Relativistic Mean Field Theory"and Fundamental Research Funds for the Central Universities(SWJTU12ZT11)
文摘The difference between the transition density of a larger mass hyperon star （for example, the neutron star PSR J1614-2230） and that of a smaller mass hyperon star is investigated in the framework of the relativistic mean field theory. We see that the transition density p0H increases with the increase of xw （i.e. the mass of the neutron star）. For the nucleons parts, the neutrons make the main contribution to the transition density as the baryon density P=p0H. With the increase of the xw （i.e. the mass of the neutron star）, the relative particle number density of neutrons decreases while that of protons increases. For the parts of hyperons, the ∧ and ≡. make the main contributions to the transition density as the baryon density p=p0H. The relative particle number density of A decreases while that of ≡ increases with the increase of the xw （i.e. the mass of the neutron star）. For the hyperons ∑-, ∑0 and E-, the total contributions are less than 16 per cent.
