In course of the consolidation of nucleon (neutron) spacing inside a compact star, two key factors are expected to come into play side by side: the lack of self-stabilization against shutting into black hole (BH) and forthcoming phase transition - color deconfinement and QCD-vacuum reconstruction - within the nuclear matter the star is composed of. These phenomena bring the star to evolve in the quite different (opposite) ways and should be taken into account at once, as the gravitational compression is considered. Under the above transition, which is expected to occur within any supermassive neutron star (NS), the hadronic-phase (HPh) vacuum - a coherent state of gluon- and chiral $q\bar q$-condensates - turns, first near the star center, into the "empty" (perturbation) subhadronic-phase (SHPh) one and, thus, pre-existing (very high) vacuum pressure falls there down rather abruptly; as a result, the "cold" star starts collapsing almost freely into the new vacuum. If the stellar mass is sufficiently large, then this implosion is shown to result in an enormous heating within the star central domain (up to a temperature about 100-200 MeV or, maybe, even higher), what makes the pressure from within to grow up, predominantly due to degeneracy breaking and multiple $q\bar q$-pair production. Thus, a "flaming wall" could arise, which withstands the further collapsing and brings the star off the irrevocable shutting into BH. Instead, the star either forms a transient quasi-steady state (just the case of relatively low star mass) and, losing its mass, evolves gradually into the "normal" steady NS, or is doomed for self-liquidation in full (at higher masses).
Hadron-quark phase transition: the QCD phase diagram and stellar conversion
不同的扩展Nambu-Jona-Lasinio模型，已知满足预期的QCD手征对称性方面，被用来调查一个可能的强子-夸克相变在零温度下，并建立相应的双结点部分。我们已经表明，过渡点是非常敏感的模型参数和压力和化学势急剧增加的矢量相互作用强度的夸克部门的增加。在同一框架下，分析了夸克和混合星形成的可能性。加强了以前关于共存压力和化学势的相同结论。我们的结论是，即使从一个亚稳态强子星到夸克星的过渡是热力学可能的，它要么是能量禁止或产生一个黑洞。尽管如此，从亚稳恒星到混合恒星的转换是可能的，但两个致密天体之间的质量差非常小，永远不会大于0.2 M $_\odot$。
Exploiting stellar explosion induced by the QCD phase transition in large-scale neutrino detectors
核心坍缩超新星的中心是宇宙中的致密环境之一。在这样的条件下，可以想象发生从普通核物质到夸克-胶子等离子体的一级相变。这种转变释放出大量的潜热，可以驱动超新星爆炸，并可能在中微子信号中留下清晰的信号。我们展示了如何捕捉功能，如果在大规模的中微子探测器观察到，可以设置竞争限制的中微子质量，并通过三角测量协助定位的超新星。95% C. L.对于距离为10 kpc的超新星，中微子质量的极限在Ice-Cube中为0.16eV，在Hyper-Kamiokande中为0.22eV，在DUNE中为0.58eV。对于相同的距离，在最乐观的中微子转换的情况下，三角测量方法可以约束的$1σ$角的不确定性的超新星定位在$\sim 0.3^{\circ}-9.0^{\circ}$内所考虑的对的检测器，从而导致改善到一个数量级的相对于经常考虑在文献中的中子化爆发的上升时间。
QCD axions and domain walls in dense matter under compact stellar conditions
Hunan University of Science and Technology（湖南科技大学）；Beihang University（北京航空航天大学）；Fudan University（复旦大学）；University of Catania（卡塔尼亚大学）；Inner Mongolia Normal University（内蒙古师范大学）
Multi-messenger signal from QCD-Axion Ultracompact Minihalos
Institut de Fìsica d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology（高能物理研究所，巴塞罗那科技研究院）；Facultad de Ingeniería, Universidad San Sebastián（圣塞巴斯蒂安大学工程学院）；Departamento de Ciencias Físicas, Universidad Andrés Bello（安德斯贝略大学物理科学系）
Asymptotic Freedom and Vacuum Polarization Determine the Astrophysical End State of Relativistic Gravitational Collapse: Quark--Gluon Plasma Star Instead of Black Hole
Colciencias National Program for Basic Sciences, Space Science（Colciencias 基础科学国家计划，空间科学）；Valencia International University（瓦伦西亚国际大学）；Escuela de Fisica, Universidad Nacional de Colombia（哥伦比亚国立大学物理学院）；Instituto de Fisica, Universidad de Antioquia（安蒂奥基亚大学物理研究所）；Department of Physics and Astronomy, West Virginia University（西弗吉尼亚大学物理与天文学系）
Bayesian constraints on quark stars from multi-messenger observations
Yuncheng University（运城大学）；Yangzhou University（扬州大学）；Tongji University（同济大学）；The Hong Kong University of Science and Technology（香港科技大学）；Peking University（北京大学）
$f$-Mode oscillations and the gravitational response of compact stars with analytic equations of state
Shanghai University（上海大学）；Shanghai Key Lab for Astrophysics（上海市天体物理重点实验室）；Shanghai Key Laboratory of High Temperature Superconductors（上海市高温超导重点实验室）；Perugia University（佩鲁贾大学）；INFN, Sezione di Perugia（意大利国家核物理研究所佩鲁贾分部）；Centro de Ciências Exatas, Naturais e Tecnológicas, UEMASUL（UEMASUL精确、自然与技术科学中心）；Departamento de Física, CCET - Universidade Federal do Maranhão（马拉尼昂联邦大学CCET物理系）；Instituto Tecnologico de Aeronautica（巴西航空技术学院）；Tamkang University（淡江大学）；National Center for Theoretical Sciences（理论科学国家中心）
Testing the QGP Star Hypothesis: The oMEGACat BH-2 System as a Candidate Color-Superconducting Quark-Gluon Plasma Star
Master Program in Astronomy and Astrophysics, Valencia International University（瓦伦西亚国际大学天文学与天体物理学硕士项目）；Colciencias, National Program for Basic Sciences/Space Science（哥伦比亚科学与技术创新局基础科学/空间科学国家项目）
General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly
Goethe Universität（法兰克福歌德大学）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文研究所）；School of Mathematics, Trinity College（都柏林三一学院数学学院）；Frankfurt Institute for Advanced Studies（法兰克福高等研究院）
Energy-momentum-squared gravity: charged quark star solutions with unified interacting matter
University of KwaZulu–Natal（夸祖鲁-纳塔尔大学）；Central Asian University（中亚大学）；University of Tashkent for Applied Sciences（塔什干应用科学大学）；Institute of Theoretical Physics, National University of Uzbekistan（乌兹别克斯坦国立大学理论物理研究所）；Tashkent International University of Education（塔什干国际教育学院）；Harbin Institute of Technology（哈尔滨工业大学）；Tongji University（同济大学）；Khazar University（哈扎尔大学）；National University of Uzbekistan（乌兹别克斯坦国立大学）；Kimyo International University in Tashkent（塔什干化学国际大学）
Post-Merger Gravitational-Wave Uncertainties of Binary Neutron Stars under Multi-Messenger EOS Constraints
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Science（暗物质与空间天文重点实验室，中国科学院紫金山天文台）；RIKEN Center for Interdisciplinary Theoretical and Mathematical Sciences (iTHEMS), RIKEN（理化学研究所跨学科理论与数学科学中心（iTHEMS））；International College and Graduate School of Science, The University of Osaka（大阪大学国际理工学部研究生院）
