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通过相对论性磁流体力学的计算知道,由双中子星合并产生的引力波对中子星内部是否存在夸克物质以及QCD物质状态方程的硬度度非常敏感.这些天文学上创造的热力学极限在20％以内跟某些快度、碰撞参数等条件下的相对论重离子碰撞产生的温度和密度相当.本文结合相对论模拟双中子星系统及实验室中重离子碰撞的结果,从而确定高密物质的状态方程和相结构.讨论了中子星合并后残留物的引力波发射,这将有助于了解夸克强子过渡的性质.“,”The gravitational waves emitted from a binary neutron star merger,as predicted from general relativistic magneto-hydrodynamics calculations,are sensitive to the appearance of quark matter and the stiffness of the equation of state of QCD matter present in the inner cores of the stars. These astrophysic-ally created extremes of thermodynamics do match,to within 20％,the values of densities and temperat-ures which are found in relativistic heavy ion collisions,if though at quite different rapidity windows,im-pact parameters and bombarding energies of the heavy nuclear systems. In this article we combine the res-ults obtained in general relativistic simulations of binary neutron star systems with ones from heavy ion collisions in the lab to pin down the EOS and the phase structure of dense matter. We discuss that the postmerger gravitational wave emission of the neutron star merger remnant might give,in the near future,insides about the properties of the hadron quark transition.