检验QGP星假说：oMEGACat BH-2系统作为色超导夸克胶子等离子体星候选体
Testing the QGP Star Hypothesis: The oMEGACat BH-2 System as a Candidate Color-Superconducting Quark-Gluon Plasma Star
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中文总结 AI 辅助
本研究以oMEGACat BH-2暗伴星的质量处于中子星与恒星级黑洞的质量间隙为切入点，探讨其为色超导QGP星的假说，发现其质量符合QGP星模型预测，提出可通过多台望远镜的天体测量与引力波观测进一步验证。
中文摘要 AI 辅助
近期在球状星团ω半人马座中发现的长周期双星系统oMEGACat BH-2（Whitaker等人，2026），为探究致密暗天体的本质提供了前所未有的机会。该系统的大质量暗伴星被推断质量为4.46+1.22−1.01 M⊙，处于中子星与恒星级黑洞的“质量间隙”之间。本文中，我们探讨以下假说：oMEGACat BH-2的伴星并非经典黑洞，而是稳定的自束缚夸克胶子等离子体（QGP）星，其由近期结合非线性电动力学（NLED）与量子色动力学（QCD）渐近自由的广义相对论模型描述（Mosquera等人，2025）。我们将该伴星的推断质量与QGP星模型预测的新型质量-半径（M-R）关系进行对比，发现该ω半人马座天体的推断质量恰好落在超大质量QGP星预测的宽质量谱（0至>7 M⊙）范围内。尽管这种一致性不足以作为证据，但它表明oMEGACat BH-2可能是首个观测到的QGP星候选体，代表恒星坍缩的稳定、无奇点终态。我们认为，未来利用詹姆斯·韦布空间望远镜（JWST）及500米口径球面射电望远镜（FAST）、平方千米阵列射电望远镜（SKA）等射电望远镜进行天体测量监测，可进一步限制oMEGACat BH-2的轨道参数；同时，利用激光干涉引力波天文台（LIGO）、室女座引力波探测器（VIRGO）、神冈引力波探测器（KAGRA）、激光干涉空间天线（LISA）、爱因斯坦望远镜（ET）、宇宙探索者（CE）等天文台对f模与g模的引力波后续观测，对区分经典黑洞与我们QGP星模型的“引力永恒坍缩‘致密’天体”（GECKO）态至关重要。
英文摘要
The recent discovery of a long-period binary system in the globular cluster $ω$ Centauri, oMEGACat BH-2 \citep{Whitaker2026}, provides an unprecedented opportunity to probe the true nature of compact dark objects. The system's massive, dark companion has been inferred to have a mass of $4.46_{-1.01}^{+1.22} M_\odot$, which places it in the ``mass gap'' between neutron stars and the canonical stellar-mass black holes. In this Letter, we explore the hypothesis that the oMEGACat BH-2 companion is not a classical black hole, but a stable, self-bound Quark-Gluon Plasma (QGP) star, as described by recent general relativistic models that incorporate Nonlinear Electrodynamics (NLED) and the asymptotic freedom of Quantum Chromodynamics (QCD) \citep{Mosquera2025}. We compare the inferred mass of the companion with the novel Mass-Radius ($M$-$R$) relation predicted by the QGP star model. We find that the inferred mass of the $ω$ Centauri object lies squarely within the wide mass spectrum predicted for hypermassive QGP stars ($0$ to $>7$ $M_\odot$). Although this consistency is not enough for claiming evidence, it suggests that oMEGACat BH-2 may be the first observed candidate for a QGP star, representing a stable, non-singular end-state of stellar collapse. We argue that future astrometric monitoring with JWST and radio-telescopes like FAST and SKA can further constrain the oMEGACat BH-2 orbital parameters. Meanwhile, gravitational-wave follow-ups for the $f$ and $g$ modes by observatories like LIGO, VIRGO, KAGRA, LISA, ET and CE can be crucial for distinguishing a classical black hole from the ``gravitational eternally collapsing `kompact' object'' (\GECKO) state of our QGP star model.
发表机构
- 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）
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