自旋极化核物质的状态方程

在Brueckner Hartree Fock理论框架内 ,研究了自旋极化核物质的状态方程及其自旋依赖性 ,计算了相关的物理量如朗道参数G0 和G′0 ,并着重讨论了三体核力的影响 .结果表明 :在整个自旋极化度范围内 ,自旋极化核物质的每核子能量随中子和质子自旋极化度的变化相当精确地满足二次方规律 ,而且在Brueckner Hartree Fock理论框架内 ,自旋非极化核物质的能量总是比相应的自旋极化核物质的能量低 ,这表明核物质中不会发生由自旋非极化态向自旋极化态的自发相变 .当密度较低时 ,三体核力对核物质状态方程的自旋依赖性的影响不明显 ;随着密度的增大 ,三体核力效应增强 ,而且三体核力使朗道参数G0 和G′0 增大 ,从而使核物质对于自旋涨落的稳定性增强

同位旋非对称核物质性质与扩展的BHF方法(Ⅶ)中子星物质中质子和中子的~1S_0态超流性

利用Brueckner Hartree Fock和BCS理论方法 ,计算了β稳定中子星物质中处于 1S0 态的质子和中子的对关联能隙 ,着重研究和讨论了三体核力的影响 .结果表明三体核力对 β稳定中子星物质中 1S0 态中子超流性的影响相对较小 ,但对 1S0 态质子超流性具有重要影响 ,而且其效应随核子数密度增大而迅速增强 .三体核力的主要作用是强烈地抑制了高密度 β稳定中子星物质中的 1S0态质子超流性 .

自旋极化中子物质的状态方程

在Brueckner-Hartree-Fock理论框架内,研究了自旋极化的中子物质的状态方程及其自旋依赖性,计算了自旋非对称能及相关的物理量如磁化率和朗道参数G_0,并着重讨论了三体核力的影响,结果表明:在整个自旋极化度范围内,中子物质的每核子能量随自旋极化度的变化都满足二次方规律,自旋对称能随密度单调增加,这意味着中子物质中不会发生由自旋非极化态向自旋极化态的自发相变,三体核力的主要效应是使中子物质磁化率随密度减小的速度加快,从而使中子物质的磁化相变更加困难。

同位旋非对称核物质性质与扩展的BHF方法(Ⅵ)质子和中子平均自由程及其同位旋依赖性

在扩展的Brueckner-Hartree-Fock理论框架内,研究了同位旋非对称核物质中质子和中子的平均自由程,着重讨论了其同位旋依赖性。结果表明:随核物质同位旋非对称度的增大,质子平均自由程减小而中子的平均自由程增大。这表明中子滴线附近的原子核表面对中子比对质子更具透明度。还简单讨论了基态关联效应对平均自由程的影响。

自旋极化的同位旋非对称核物质性质

利用Skyrme有效相互作用 ,采用核子 -核子相互作用参数SKM 和SⅢ对自旋极化的同位旋非对称核物质的特性和状态方程进行了研究 ,讨论了非对称核物质的磁化率随密度的变化关系及其同位旋依赖性 .结果表明 :在Skyrme Hartree Fock框架内 ,同位旋非对称核物质会发生从非极化态到极化态的相变 ,而且发生相变的临界密度随同位旋非对称度增大而降低 .另外 ,还与微观BHF (Brueckner Hartree Fock)的理论预言进行了比较和讨论

同位旋非对称核物质性质与扩展的BHF方法(Ⅴ)三体核力对质子和中子单粒子势的影响

在扩展的同位旋相关的Brueckner Hartree Fock理论框架内 ,研究了三体核力对同位旋非对称核物质中质子与中子的单粒子势及其同位旋依赖性的影响 .

同位旋非对称核物质性质与扩展的BHF方法(Ⅳ)单粒子势与有效质量

在扩展的同位旋相关的Brueckner Hartree Fock理论框架内 ,计算了同位旋非对称核物质中质子与中子的单粒子势和有效质量及其同位旋效应 ,并详细研究和讨论了基态关联对单粒子势和有效质量及其同位旋依赖的影响

同位旋非对称核物质性质与扩展的BHF方法(Ⅰ)同位旋相关的扩展的BHF方法

通过引进基态关联和同位旋自由度的区分 ,推广了Brueckner Hartree Fock理论方法 ,并应用于同位旋非对称核物质 ,系统地研究了在整个同位旋自由度范围内核物质的状态方程和单粒子特性及其同位旋效应 .还研究了微观三体核力对同位旋非对称核物质性质及其同位旋效应的影响 ,定量讨论了三体力效应与相对论性平均场理论及Dirac Brueckner方法的联系 .主要给出了同位旋相关的Brueckner Hartree Fock方法的基本理论和计算公式

中子物质中超流性的自能色散效应

利用扩展的 Brueckner- Hartree- Fock理论与推广的 BCS方法研究了自能的色散效应和基态关联对中子物质中超流性和能隙的影响 .研究结果表明 ,自能的色散效应使中子物质中能隙减小 ;考虑基态关联后 ,超流性将进一步减弱 .

Isospin dependence of nucleon (PF2)-P-3 superfluidity in asymmetric nuclear matter

We have investigated the isospin dependence of the neutron and proton (PF2)-P-3 superfluidity in isospin-asymmetric nuclear matter within the framework of the Brueckner-Hartree-Fock approach and the BCS theory. We show that the (PF2)-P-3 neutron and proton pairing gaps depend sensitively on isospin asymmetry of asymmetric nuclear matter. As the isospin asymmetry increases, the neutron (PF2)-P-3 superfluidity becomes stronger and the peak value of the neutron (PF2)-P-3 pairing gap increases rapidly. The isospin dependence of the proton (PF2)-P-3 superfluidity is shown to be opposite to the neutron one. The proton (PF2)-P-3 superfluidity becomes weaker at a higher asymmetry and it even vanishes at high enough asymmetries. At high asymmetries, the neutron (PF2)-P-3 superfluidity turns out to be much stronger than the proton one, implying that the neutron (PF2)-P-3 superfluidity is dominated in the highly asymmetric dense interior of neutron stars.

Microscopic Three-Body Force Effect on Nucleon-Nucleon Cross Sections in Symmetric Nuclear Matter

We provide a microscopic calculation of neutron-proton and proton-proton cross sections in symmetric nuclear matter at various densities, using the Brueckner-Hartee-Fock approximation scheme with the Argonne V-14 potential including the contribution of microscopic three-body force. We investigate separately the effects of three-body force on the effective mass and on the scattering amplitude. In the present calculation, the rearrangement contribution of three-body force is considered, which will reduce the neutron and proton effective mass, and depress the amplitude of cross section. The effect of three body force is shown to be repulsive, especially in high densities and large momenta, which will suppress the cross section markedly.

Hot Nuclear Matter Equation of State and Finite Temperature Kaon Condensation

We perform a systematic calculation of the equation of state of asymmetric nuclear matter at finite temperature within the framework of the Brueckner-Hartree-Fock approach with a microscopic three-body force. When applying it to the study of hotka on condensed matter, we find that the thermal effect is more profound in comparison with normal matter, in particular around the threshold density. Also, the increase of temperature makes the equation of state slightly stiffer through suppression of kaon condensation.

Consistent nucleon-nucleon potentials and three-body forces

We construct microscopic three-nucleon forces consistent with the Bonn and Nijmegen two-nucleon potentials, and including , Roper, and nucleon-antinucleon excitations. Recent results for the choice of the meson parameters are discussed. The forces are used in Brueckner calculations and the saturation properties of nuclear matter are determined.

Three-body force effect on P-3 F-2 neutron superfluidity in neutron matter, neutron star matter, and neutron stars

We investigate the effect of microscopic three-body forces on the P-3 F-2 neutron superfluidity in neutron matter, beta-stable neutron star matter, and neutron stars by using the BCS theory and the Brueckner-Hartree-Fock approach. We adopt the Argonne V18 potential supplemented with a microscopic three-body force as the realistic nucleon-nucleon interaction. We have concentrated on studying the three-body force effect on the P-3 F-2 neutron pairing gap. It is found that the three-body force effect considerably enhances the P-3 F-2 neutron superfluidity in neutron star matter and neutron stars.

(PF2)-P-3 neutron superfluidity in neutron stars and three-body force effect

We investigate the (PF2)-P-3 neutron superfluidity in beta-stable neutron star matter and neutron stars by using the BCS theory and the Brueckner-Hartree-Fock approach. We adopt the Argonne V-18 potential supplemented with a microscopic three-body force as the realistic nucleon-nucleon interaction. We have concentrated on studying the three-body force effect on the (PF2)-P-3 neutron pairing gap. It is found that the three-body force effect is to enhance remarkably the (PF2)-P-3 neutron superfluidity in neutron star matter and neutron stars.