GW190814背景下强子-夸克相变

I. A. Rather, A. A. Usmani, S. Patra
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引用次数: 14

摘要

在密度相关相对论平均场模型(DD-RMF)中计算了强子物质的中子星性质。研究了夸克物质的相变过程,并利用矢量增强袋模型(vBag)系统地计算了混合星物质的性质。采用Gibbs和Maxwell两种构造方法,发现具有DD-LZ1和DD-RMF参数集的中子星在纯强子相时的最大质量约为2.55 $M_{\odot}$,在强子-夸克混合相时的最大质量约为2 $M_{\odot}$。在1.4 $M_{\odot}$, $\Lambda_{1.4}$处,杂化EoS的潮汐变形能力与麦克斯韦构造的纯强子EoS相比保持不变,但随着吉布斯构造中子星质量的增加而降低。纯强子物质EoS满足最近观测到的GW190814数据的质量约束,而强子-夸克相变的恒星物质性质满足最近观测到的GW170817的约束。因此,我们不能排除GW190814中的次级天体是由强子和夸克组成的中子星的可能性。
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Hadron–quark phase transition in the context of GW190814
The properties of the neutron stars are calculated for the hadronic matter within the density-dependent relativistic mean-field model (DD-RMF). The phase transition to the quark matter is studied and the hybrid star matter properties are systematically calculated using the Vector-Enhanced Bag model (vBag). The maximum mass of neutron star with DD-LZ1 and DD-RMF parameter sets is found to be around 2.55$M_{\odot}$ for pure hadronic phase and around 2$M_{\odot}$ for hadron-quark mixed phase using both Gibbs and Maxwell construction. The tidal deformability for the hybrid EoS at 1.4$M_{\odot}$, $\Lambda_{1.4}$, remains unchanged from the pure hadronic EoS with Maxwell construction, but decreases with the increasing neutron star mass for Gibbs construction. While the pure hadron matter EoS satisfies the mass constraint from recently observed GW190814 data, the star matter properties for the hadron-quark phase transition satisfy the constraints from the recent observations GW170817. Therefore, we cannot exclude the possibility of the secondary object in GW190814 as a neutron star composed of hadrons and quarks.
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