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This letter tests whether the companion is a stable, self-bound Quark-Gluon Plasma (QGP) star using general-relativistic models with Nonlinear Electrodynamics (NLED) and QCD asymptotic freedom, comparing inferred mass with a QGP mass-radius relation and assessing future astrometric and gravitational-wave discrimination.",{"@graph":14,"@context":73},[15,34,56],{"@type":16,"itemListElement":17},"BreadcrumbList",[18,23,27,31],{"item":19,"name":20,"@type":21,"position":22},"https://docshare.wps.com","Home","ListItem",1,{"item":24,"name":25,"@type":21,"position":26},"https://docshare.wps.com/document/","Document",2,{"item":28,"name":29,"@type":21,"position":30},"https://docshare.wps.com/document/research-report/","Research & 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Sterling","Person",{"url":19,"name":45,"@type":46},"DocShare","Organization","application/pdf","2026-11-06","2026-09-15",true,{"@type":52,"interactionType":53,"userInteractionCount":55},"InteractionCounter",{"@type":54},"ViewAction",17,{"@type":57,"mainEntity":58},"FAQPage",[59,65,69],{"name":60,"@type":61,"acceptedAnswer":62},"What hypothesis does the paper test about the oMEGACat BH-2 companion?","Question",{"text":63,"@type":64},"It tests whether the oMEGACat BH-2 companion is a stable, self-bound Quark-Gluon Plasma (QGP) star rather than a classical black hole.","Answer",{"name":66,"@type":61,"acceptedAnswer":67},"How is the companion mass used to evaluate the QGP star model?",{"text":68,"@type":64},"The inferred companion mass is compared against the novel QGP star mass-radius relation and the predicted hypermassive QGP mass spectrum.",{"name":70,"@type":61,"acceptedAnswer":71},"What observations are proposed to further constrain or distinguish the nature of oMEGACat BH-2?",{"text":72,"@type":64},"Future astrometric monitoring with JWST and radio telescopes such as FAST and SKA are proposed, along with gravitational-wave follow-ups for relevant oscillation modes using LIGO, VIRGO, KAGRA, LISA, ET, and CE.","https://schema.org",{"og:url":32,"og:type":75,"og:title":10,"og:site_name":45,"og:description":12},"article",{"robots":77,"canonical":32},"index,follow",{"doc_id":79,"site_id":7},269357,1789450910,{"code":4,"msg":82,"data":83},"success",[84,88,92,96,101,106,111,115,120,123,127],{"id":22,"doc_module":4,"doc_module_name":25,"category_name":85,"show_sort_weight":86,"slug":87},"Story & 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LATEX twocolumn style in AASTeX631  \nTesting the QGP Star Hypothesis: The oMEGACat BH-2 System as a Candidate Color-Superconducting Quark-Gluon Plasma Star  \nHerman J. Mosquera Cuesta  1, 2  \n1 Master Program in Astronomy and Astrophysics, Valencia International University, C/ Pintor Sorolla, 21, 46002, Valencia, Spain 2 Visiting Scientist Colciencias, National Program for Basic Sciences/Space Science, Avenida Calle 26, No. 57-41 Torre 8, Pisos 2-6,  \nBogota, Colombia. Corresponding author: a  \nABSTRACT  \nThe recent discovery of a long-period binary system in the globular cluster ω Centauri, oMEGACat BH-2 (Whitaker et al. 2026), 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  \n4.4611..2201M⊙ , 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) (Mosquera Cuesta et al. 2025) . We compare the inferred mass of the companion with the novel Mass-Radius (M-R) relation predicted by the QGP star model.  \nWe 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⊙ ) . 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  \noMEGACat 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.  \nKeywords: Stellar mass black holes (1611); Black holes (162); Globular star clusters (656); Astrometric binary stars (79); Binary stars (154); Quark stars (3058); Nonlinear electrodynamics; Quantum chromodynamics  \n1. INTRODUCTION  \nThe modern view of astrophysics is built upon the concept of the black hole. However, the singularity theorem predictions of General Relativity (GR) remain a fundamental theoretical challenge (Kerr 2023) . The last decade’s breakthroughs—from the discovery of gravitational waves (Abbott et al. 2016) to the detection of Quark-Gluon Plasma (QGP) and light-by-light scattering at the LHC (ATLAS Collaboration 2017; ALICE Collaboration 2020)—provide a powerful motivation torevisit the ultimate state of relativistic gravitational collapse.  \n[a](a herman@icra.it)[ herman@icra.it](a herman@icra.it)  \nWe have developed a model of a hypermassive, extremely magnetized QGP star that is supported against collapse by a combination of the repulsive vacuum polarization pressure from Nonlinear Electrodynamics (NLED) and the asymptotic freedom of QCD (Mosquera Cuesta et al. 2025) . This object is self-bound, has a finite radius always exceeding its Schwarzschild radius, and can mimic the gravitational behavior of a black hole. In this paper, we test this hypothesis against the recent observational discovery of a dark, massive companion in the globular cluster ω Centauri.  \n2. THE OBSERVATIONAL ANCHOR: THE  \nOMEGACAT BH-2 SYSTEM  \nThe recent discovery of oMEGACat BH-2 in ω Centauri (Whitaker et al. 2026) is the first astrometric dis-  \n2  \ncovery of a black hole in a globular cluster. The key observational facts are:  \n2.1. Astrometric Measurements  \nUsing HST and JW","cbCaimTfjxnaoDAP","https://ap.wps.com/l/cbCaimTfjxnaoDAP","pdf",1072909,"English","# ABSTRACT\n# 1. INTRODUCTION\n# 2. THE OBSERVATIONAL ANCHOR: THE OMEGACAT BH-2 SYSTEM\n## 2.1. Astrometric Measurements\n## 2.2. Orbital Fit\n## 2.3. Companion Mass\n# 3. THE QGP STAR MODEL: A THEORETICAL ALTERNATIVE\n## 3.1. The Modified TOV Equation","[{\"question\":\"What hypothesis does the paper test about the oMEGACat BH-2 companion?\",\"answer\":\"It tests whether the oMEGACat BH-2 companion is a stable, self-bound Quark-Gluon Plasma (QGP) star rather than a classical black hole.\"},{\"question\":\"How is the companion mass used to evaluate the QGP star model?\",\"answer\":\"The inferred companion mass is compared against the novel QGP star mass-radius relation and the predicted hypermassive QGP mass spectrum.\"},{\"question\":\"What observations are proposed to further constrain or distinguish the nature of oMEGACat BH-2?\",\"answer\":\"Future astrometric monitoring with JWST and radio telescopes such as FAST and SKA are proposed, along with gravitational-wave follow-ups for relevant oscillation modes using LIGO, VIRGO, KAGRA, LISA, ET, and CE.\"}]","Testing the QGP Star Hypothesis - The oMEGACat BH-2 System as a Candidate Color-Superconducting Quark-Gluon Plasma Star | PDF",18]