The properties of neutron stars are calculated for hadronic matter within the density-dependent relativistic mean-field model (DD-RMF). The phase transition to quark matter is studied and the hybrid star matter properties are systematically calculated using the vector-enhanced bag model. The maximum mass of a neutron star with DD-LZ1 and DD-RMF parameter sets is found to be around 2.55M _⊙ for the pure hadronic phase and around 2M _⊙ for the hadron–quark mixed phase using both Gibbs and Maxwell construction (MC). The variation in tidal deformability for the hybrid equation of state (EoS) at 1.4M _⊙ depends upon the construction of the phase transition. While it remains unchanged with MC, but decreases with the increasing neutron star mass for Gibbs construction. The pure hadron matter EoS satisfies the maximum mass constraint from recently observed GW190814 data, implying a stiff neutron star EoS. The phase transition to quark matter satisfies the maximum mass and radius constraints from the GW170817 event. Therefore, we cannot exclude the possibility of the secondary object in GW190814 as a neutron star with a phase transition to quark matter that satisfies the 2M _⊙ maximum mass limit.

中子星的属性是在密度相关相对论平均场模型 (DD-RMF) 中计算强子物质的。研究了夸克物质的相变，并使用矢量增强袋模型系统地计算了混合星物质的特性。中子星与DD-LZ1和DD-RMF参数集的最大质量被发现是围绕2.55中号 _⊙为纯强子相和大约2中号 _⊙同时使用吉布斯和麦克斯韦结构强子夸克混合相（MC ）。混合状态方程 (EoS) 在 1.4 M 处潮汐变形能力的变化_⊙取决于相变的构造。虽然它与 MC 保持不变，但随着吉布斯构造的中子星质量的增加而减少。纯强子物质 EoS 满足最近观测到的 GW190814 数据的最大质量约束，这意味着刚性中子星 EoS。夸克物质的相变满足 GW170817 事件的最大质量和半径约束。因此，我们不能排除 GW190814 中的次生天体是一颗中子星的可能性，其相变为满足 2 M _⊙最大质量限制的夸克物质。