论文标题
根据GW170817查找中子星的夸克含量
Finding quark content of neutron stars in light of GW170817
论文作者
论文摘要
GW170817的重力波的检测为限制了中子星的状态（EOS）方程提供了新的机会。在本文中，我们研究了GW170817的背景下中子星核内夸克的可能存在。在我们采用了一系列可用模型的相对论核均值场方法中，对核子相进行了处理，并且在袋模型中描述了夸克相。我们表明，当允许通过Gibbs的构造向夸克物质转变为Quark物质时，与潮汐变形性结合不一致的核子EOSS变得一致。我们发现，几个核酸eoss支持纯夸克物质核心的存在，而小质量不超过$ 0.17亿美元\ odot $，而半径为0.9 km。我们还发现，即使在核素Quark相变的潮汐变形性与中子星形半径之间的强度相关性也持续存在，并且在$ R_ {1.4} \ lyssim 12.9 $ 12.9 $ km的半径上提供了上限，价格为1400万美元\ odot $ natron $ natron $ netron $ natron $中性恒星。
The detection of gravitational waves from GW170817 has provided a new opportunity to constrain the equation of state (EOS) of neutron stars. In this article, we investigate the possible existence of quarks inside the neutron star core in the context of GW170817. The nucleon phase is treated within the relativistic nuclear mean-field approach where we have employed a fully comprehensive set of available models, and the quark phase is described in the Bag model. We show that the nucleonic EOSs which are inconsistent with the tidal deformability bound become consistent when phase transition to quark matter via Gibbs construction is allowed. We find that several nucleonic EOSs support the presence of pure quark matter core with a small mass not more than $0.17M_\odot$ confined within a radius of 0.9 km. We also find that the strong correlation between tidal deformability and neutron star radii observed for pure nucleonic stars does persist even with a nucleon-quark phase transition and provides an upper limit on the radius of $R_{1.4} \lesssim 12.9$ km for a $1.4M_\odot$ neutron star.
