通过六夸克凝聚实现致密星中的夸克解禁闭
Quark deconfinement in compact stars through sexaquark condensation
AI总结：
本文首次提出轻六夸克的玻色-爱因斯坦凝聚触发致密星早期夸克解禁闭，并发展三味密度泛函模型描述色-味锁定相，揭示强相互作用物质中的BEC-BCS转变。
摘要：
在这项贡献中，我们首次提出一种情形：致密星中的早期夸克解禁闭由质量为 $m_S<2054$ MeV 的轻六夸克（S）的玻色-爱因斯坦凝聚（BEC）触发，该粒子曾被建议作为解释宇宙中重子暗物质的候选粒子。S 的 BEC 开始标志着强子中子星的最大质量，并且当恒星中心满足重子化学势条件 $μ_b=m_S/2$ 时发生，对应的起始质量 $M_{\rm onset}\lesssim 0.7~M_\odot$。在恒星的引力场中，S 的 BEC 密度不断增加，直到达到一种新的物质状态，此时每个 S 态解离为三重色-味锁定（CFL）双夸克态。这些双夸克是夸克物质色超导 CFL 相中的库珀对，因此所发展的情形对应于强相互作用物质中的 BEC-BCS 转变。为了描述 CFL 相，我们在此首次发展了三味扩展的密度泛函公式，该公式基于手征对称拉格朗日夸克物质模型，其中禁闭性质被编码为标量自能在低密度和低温下的发散。
英文摘要：
In this contribution, we present for the first time a scenario according to which early quark deconfinement in compact stars is triggered by the Bose-Einstein condensation (BEC) of a light sexaquark (S) with a mass $m_S<2054$ MeV, that has been suggested as a candidate particle to explain the baryonic dark matter in the Universe. The onset of S BEC marks the maximum mass of hadronic neutron stars and it occurs when the condition for the baryon chemical potential $μ_b=m_S/2$ is fulfilled in the center of the star, corresponding to $M_{\rm onset}\lesssim 0.7~M_\odot$. In the gravitational field of the star the density of the BEC of the S increases until a new state of the matter is attained, where each of the S-states got dissociated into a triplet of color-flavor-locked (CFL) diquark states. These diquarks are the Cooper pairs in the color superconducting CFL phase of quark matter, so that the developed scenario corresponds to a BEC-BCS transition in strongly interacting matter. For the description of the CFL phase, we develop here for the first time the three-flavor extension of the density-functional formulation of a chirally symmetric Lagrangian model of quark matter where confining properties are encoded in a divergence of the scalar self-energy at low densities and temperatures.
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