标题： 从半微观状态方程中得到的中子星和大质量脉冲星的潮汐变形性和致密性 显示英文标题

标题： Tidal deformability and compactness of neutron stars and massive pulsars from semi-microscopic equations of state

摘要： 潮汐可变形性衡量中子星在受到施加的潮汐场作用时能够舒适变形的程度。 我们使用对中子星（NS）天体和脉冲星的质量、半径和潮汐可变形性的更新约束，来检验基于现实有限范围M3Y核子-核子相互作用的核方程状态（EOS），这些EOS已被成功用于描述低密度和高密度核物质（NM）。 然后，我们利用这些EOS来检验中子星的潮汐可变形性和致密性对其结构的影响。 我们发现，具有饱和压缩性${K}_{0}=230-330$MeV 的从 CDM3Y-230 到 CDM3Y-330 的 EOS，相比实验推导的范围，为中子星天体提供了更有限的潮汐可变形性和半径范围。 对于轻质量的 NS（$M<\text{M}_{\odot}$），当 NS 质量减小时，${k}_{2}$和$\mathcal{C}$都会减少，这增强了其潮汐可变形性。 中子星核心物质的刚度对这种 NS 的潮汐可变形性表现出轻微的影响（$M<\text{M}_{\odot}$）。 当增加（减少）所采用的 EOS 的刚度（其质量）时，得到相反的行为，即潮汐洛夫数增加而中子星的更有效的致密性减少（$M>\text{M}_{\odot}$）。 这表现为在更致密的 NM 中的中子星以及较轻的 NS 上，由于更大的半径而显示出增强的潮汐可变形性（$\text{M}_{\odot}$）。 提供了一种统一的描述，说明潮汐可变形性、潮汐洛夫数和 NS 致密性之间的一些相关性，而不依赖于所考虑 EOS 的细节。 显示英文摘要

摘要： Tidal deformability measures how NS can comfortably deform as a response to an applied tidal field. We use updated constraints on the mass, radius, and tidal deformability of neutron star (NS) objects and pulsars to examine nuclear equations of state (EOS) based on realistic finite-range M3Y nucleon-nucleon interaction, which have been successfully used to describe low- and high-dense nuclear matter (NM). We then employ these EOSs to examine the impact of tidal deformability and compactness of NSs on their structure. We found that the EOSs from CDM3Y-230 to CDM3Y-330 characterized with the saturation incompressibility ${K}_{0}=230-330$ MeV together yield more limited ranges of tidal deformability and radius for NS objects than their experimentally inferred ranges. For light NS ($M<\text{M}_{\odot}$), both ${k}_{2}$ and $\mathcal{C}$ decreases upon decreasing the NS mass, which enhances its tidal deformability. The stiffness of the NS core matter has shown a minor effect on the tidal deformability of such NS ($M<\text{M}_{\odot}$). An opposite behavior is obtained as an increase in the tidal Love number but a decrease in the more effective compactness of NS ($M>\text{M}_{\odot}$), upon increasing (decreasing) the stiffness of the employed EOS (its mass). This appears as enhanced tidal deformability indicated at a larger radius for NS of stiffer NM and for the lighter NS above $\text{M}_{\odot}$. Unified description of some correlations between tidal deformability, tidal Love number, and NS compactness is provided independent of the details of the considered EOS.