论文标题
自旋对称能和自旋偏振中子星形物质的状态方程
Spin symmetry energy and equation of state of spin-polarized neutron star matter
论文作者
论文摘要
使用依赖依赖性的核子核子相互作用，研究了在Hartree-cock（HF）形式上研究自旋偏振核物质（NM）的状态（EOS）的方程。使用NM中的自旋偏振重子元的非零分数$δ$，HF能量密度的自旋和自旋质量依赖性部分产生\ emph {旋转对称性}能量，其表现与\ emph {Isospin Symmetry}能量的方式大致相同，在文献中广泛讨论了核对称能量。目前的HF研究表明，在整个重子密度范围内，自旋对称能量与核对称能量之间存在很强的相关性。发现自旋对称能对自旋偏振NM的EOS的重要贡献与核对称能的核对称能量与等异种极化或不对称或不对称（中子）NM的EOS相当。基于HF能量密度，获得自旋（$β$稳定）NP $eμ$的EOS用于测定中子星（NS）的宏观特性。有人建议使用自旋分数$δ$的逼真的密度依赖性，以探索自旋对称能量对重力质量$ m $和半径$ r $的影响，以及NS的潮汐变形性。 Given the empirical constrains inferred from a coherent Bayesian analysis of gravitational wave signals of the NS merger GW170817 and the observed masses of the heaviest pulsars, the strong impacts of the spin symmetry energy $W$, nuclear symmetry energy $S$, and nuclear incompressibility $K$ to the EOS of nucleonic matter in magnetar were revealed.
Equation of states (EOS) of the spin-polarized nuclear matter (NM) is studied within the Hartree-Fock (HF) formalism using the realistic density dependent nucleon-nucleon interaction. With a nonzero fraction $Δ$ of spin-polarized baryons in NM, the spin- and spin-isospin dependent parts of the HF energy density give rise to the \emph{spin symmetry} energy that behaves in about the same manner as the \emph{isospin symmetry} energy, widely discussed in literature as the nuclear symmetry energy. The present HF study shows a strong correlation between the spin symmetry energy and nuclear symmetry energy over the whole range of baryon densities. The important contribution of the spin symmetry energy to the EOS of the spin-polarized NM is found to be comparable with that of the nuclear symmetry energy to the EOS of the isospin-polarized or asymmetric (neutron-rich) NM. Based on the HF energy density, the EOS of the spin-polarized ($β$-stable) np$eμ$ matter is obtained for the determination of the macroscopic properties of neutron star (NS). A realistic density dependence of the spin-polarized fraction $Δ$ have been suggested to explore the impact of the spin symmetry energy to the gravitational mass $M$ and radius $R$, as well as the tidal deformability of NS. Given the empirical constrains inferred from a coherent Bayesian analysis of gravitational wave signals of the NS merger GW170817 and the observed masses of the heaviest pulsars, the strong impacts of the spin symmetry energy $W$, nuclear symmetry energy $S$, and nuclear incompressibility $K$ to the EOS of nucleonic matter in magnetar were revealed.
