Asymptotic Freedom and Vacuum Polarization Determine the Astrophysical End State of Relativistic Gravitational Collapse: Quark--Gluon Plasma Star Instead of Black Hole
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| Formato: | Preprint |
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2026
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| _version_ | 1866917254794313728 |
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| author | Cuesta, Herman J. Mosquera Giraldo, Fabián H. Zuluaga Pardo, Wilmer D. Alfonso Santrich, Edgardo Marbello Franco, Guillermo U. Avendaño Larrazabal, Rafael Fragozo |
| author_facet | Cuesta, Herman J. Mosquera Giraldo, Fabián H. Zuluaga Pardo, Wilmer D. Alfonso Santrich, Edgardo Marbello Franco, Guillermo U. Avendaño Larrazabal, Rafael Fragozo |
| contents | A general relativistic model of an astrophysical hypermassive extremely magnetized ultra-compact self-bound quark--gluon plasma object that is supported against its ultimate gravitational implosion by the simultaneous action of the vacuum polarization driven by nonlinear electrodynamics (NLED: light-by-light scattering) and the quantum chromodynamics (QCD) asymptotic freedom, is presented. These QCD stars can be the final figures of the equilibrium of collapsing stellar cores. Post-supernova fallback material pushes the nascent remnant beyond its stability to collapse into a hybrid hypermassive neutron star (HHMNS). Hypercritical accretion can unbind the whole HHMNS's baryons to spontaneously break away color confinement, powering a first-order hadron-to-quark phase transition to a sea of ever-freer quarks and gluons. This core is hydro-stabilized by the steady, endlessly compression-admitting asymptotic freedom state, possibly via gluon-mediated enduring exchange of color charge among bound states. The nonlinear TOV equation indicates the occurrence of hypermassive QGP/QCD stars with a wide mass spectrum ($0\lesssim$ M$^{\rm{QGP}}_{\rm{Star}}\lesssim$\,7\,M$_\odot$ and beyond), for star radii ($0\lesssim R^{\rm{QGP}}_{\rm{Star}}\lesssim 24$\,km and beyond) with B-fields ($10^{14} \leq$ B$^{\rm{QGP}}_{\rm{Star}} \leq 10^{16}$\,G and beyond). Such QCD stars can emulate what the true black holes are supposed to gravitationally do in most astrophysical settings. This color quark star could be found through a search for its eternal ``yo-yo'' state gravitational-wave emission, or via lensing phenomena like gravitational rainbows, as in this scenario it is expected that the light deflection angle, directly influenced by the larger effective mass/radius and magnetic field of the deflecting object, increases as the incidence angle decreases for impact parameter lower values. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_07004 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Asymptotic Freedom and Vacuum Polarization Determine the Astrophysical End State of Relativistic Gravitational Collapse: Quark--Gluon Plasma Star Instead of Black Hole Cuesta, Herman J. Mosquera Giraldo, Fabián H. Zuluaga Pardo, Wilmer D. Alfonso Santrich, Edgardo Marbello Franco, Guillermo U. Avendaño Larrazabal, Rafael Fragozo General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena High Energy Physics - Phenomenology Nuclear Theory A general relativistic model of an astrophysical hypermassive extremely magnetized ultra-compact self-bound quark--gluon plasma object that is supported against its ultimate gravitational implosion by the simultaneous action of the vacuum polarization driven by nonlinear electrodynamics (NLED: light-by-light scattering) and the quantum chromodynamics (QCD) asymptotic freedom, is presented. These QCD stars can be the final figures of the equilibrium of collapsing stellar cores. Post-supernova fallback material pushes the nascent remnant beyond its stability to collapse into a hybrid hypermassive neutron star (HHMNS). Hypercritical accretion can unbind the whole HHMNS's baryons to spontaneously break away color confinement, powering a first-order hadron-to-quark phase transition to a sea of ever-freer quarks and gluons. This core is hydro-stabilized by the steady, endlessly compression-admitting asymptotic freedom state, possibly via gluon-mediated enduring exchange of color charge among bound states. The nonlinear TOV equation indicates the occurrence of hypermassive QGP/QCD stars with a wide mass spectrum ($0\lesssim$ M$^{\rm{QGP}}_{\rm{Star}}\lesssim$\,7\,M$_\odot$ and beyond), for star radii ($0\lesssim R^{\rm{QGP}}_{\rm{Star}}\lesssim 24$\,km and beyond) with B-fields ($10^{14} \leq$ B$^{\rm{QGP}}_{\rm{Star}} \leq 10^{16}$\,G and beyond). Such QCD stars can emulate what the true black holes are supposed to gravitationally do in most astrophysical settings. This color quark star could be found through a search for its eternal ``yo-yo'' state gravitational-wave emission, or via lensing phenomena like gravitational rainbows, as in this scenario it is expected that the light deflection angle, directly influenced by the larger effective mass/radius and magnetic field of the deflecting object, increases as the incidence angle decreases for impact parameter lower values. |
| title | Asymptotic Freedom and Vacuum Polarization Determine the Astrophysical End State of Relativistic Gravitational Collapse: Quark--Gluon Plasma Star Instead of Black Hole |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena High Energy Physics - Phenomenology Nuclear Theory |
| url | https://arxiv.org/abs/2602.07004 |