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2026
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| Online Access: | https://doi.org/10.5281/zenodo.18434918 |
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| _version_ | 1866901577357328384 |
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| author | Kulkarni, Raghu |
| author_facet | Kulkarni, Raghu |
| contents | <p>Current observations of Neutron Stars present a conflict between Gravitational Wave data</p> <p>(GW170817), which favors a compact “soft” Equation of State (R ≈ 11.5− 12.0 km), and X-</p> <p>ray Pulse Profiling (NICER), which reports systematically larger radii (R ≈ 13 km). We pro-</p> <p>pose that this “Radius Tension” is not a nuclear physics contradiction, but a geometric signature</p> <p>of the vacuum lattice transitioning from a coordination number of K = 12 (bulk) to K = 13</p> <p>(surface). Unlike black holes, where the vacuum transition is gravitationally dampened, neu-</p> <p>tron stars are supported by degeneracy pressure, allowing the full topological expansion ratio</p> <p>(ξ = 13/12 ≈ 1.0833) to manifest. This zero-parameter model accurately predicts the observed</p> <p>radius of PSR J0030+0451 (12.0 km × 1.0833 ≈ 13.0 km) and the maximum mass saturation limit</p> <p>of PSR J0952-0607 (2.17M<span>⊙ </span>×1.0833 ≈ 2.35M<span>⊙</span>), effectively resolving the tension without invoking</p> <p>exotic matter.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_18434918 |
| institution | Zenodo |
| language | |
| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | Resolution of the Neutron Star Radius and Mass Anomalies via Geometric Vacuum Sintering Kulkarni, Raghu <p>Current observations of Neutron Stars present a conflict between Gravitational Wave data</p> <p>(GW170817), which favors a compact “soft” Equation of State (R ≈ 11.5− 12.0 km), and X-</p> <p>ray Pulse Profiling (NICER), which reports systematically larger radii (R ≈ 13 km). We pro-</p> <p>pose that this “Radius Tension” is not a nuclear physics contradiction, but a geometric signature</p> <p>of the vacuum lattice transitioning from a coordination number of K = 12 (bulk) to K = 13</p> <p>(surface). Unlike black holes, where the vacuum transition is gravitationally dampened, neu-</p> <p>tron stars are supported by degeneracy pressure, allowing the full topological expansion ratio</p> <p>(ξ = 13/12 ≈ 1.0833) to manifest. This zero-parameter model accurately predicts the observed</p> <p>radius of PSR J0030+0451 (12.0 km × 1.0833 ≈ 13.0 km) and the maximum mass saturation limit</p> <p>of PSR J0952-0607 (2.17M<span>⊙ </span>×1.0833 ≈ 2.35M<span>⊙</span>), effectively resolving the tension without invoking</p> <p>exotic matter.</p> |
| title | Resolution of the Neutron Star Radius and Mass Anomalies via Geometric Vacuum Sintering |
| url | https://doi.org/10.5281/zenodo.18434918 |