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2026
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| Online Access: | https://doi.org/10.5281/zenodo.18896991 |
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| _version_ | 1866902168095686656 |
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| author | Kulkarni, Raghu |
| author_facet | Kulkarni, Raghu |
| contents | <p>StandardsemiclassicalgravitypredictsthatblackholesevaporateviaHawkingradiationwith</p> <p>a lifetime scaling of τ ∝M<span>3 </span>[<span>1</span>]. This slow decay rate imposes strict constraints on the abun-</p> <p>dance of Primordial Black Holes (PBHs), as those formed in the early universe (M∼10<span>15 </span>g)</p> <p>would persist today, conflicting with gamma-ray background observations [<span>2</span>]. We propose</p> <p>an alternative decay mechanism based on the Selection-Stitch Model (SSM) [<span>3</span>], where the</p> <p>vacuum is modeled as a discrete Face-Centered Cubic (FCC) tensor network. By recognizing</p> <p>the 3D bulk as an isometric holographic projection of a continuous 2D boundary, the vacuum</p> <p>functions as an Isometric Tensor Network (isoTNS) [<span>4</span>]. This mathematical structure retains</p> <p>genuine mechanical properties (domain walls and discrete tension) while simultaneously pre-</p> <p>serving exact Lorentz invariance. Treating the event horizon as a topological vacancy, we</p> <p>apply the Allen-Cahn equation [<span>5</span>] alongside quantum rate theory to derive a "Geometric</p> <p>Evaporation" mode driven by physical lattice tension. We analytically derive a recession</p> <p>velocity of˙</p> <p>R=−(c/2)(l<span>P </span>/R<span>H </span>), yielding a much faster decay law of τ ∝M<span>2</span>. Quantita-</p> <p>tively, a 10<span>15 </span>g PBH evaporates in 0.45 milliseconds via this geometric channel, compared</p> <p>to∼14 billion years via Hawking radiation. A discrete Peierls Locking mechanism with a</p> <p>correlation length of L<span>corr </span>∼1 fm ensures that this rapid channel cleanly eradicates micro-</p> <p>scopic PBHs while exponentially shutting off to leave macroscopic astrophysical black holes</p> <p>perfectly stable.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_18896991 |
| institution | Zenodo |
| language | |
| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | Geometric Evaporation: Solving the Primordial Black Hole Constraint via Lattice Tension in an Isometric Holographic Vacuum Kulkarni, Raghu <p>StandardsemiclassicalgravitypredictsthatblackholesevaporateviaHawkingradiationwith</p> <p>a lifetime scaling of τ ∝M<span>3 </span>[<span>1</span>]. This slow decay rate imposes strict constraints on the abun-</p> <p>dance of Primordial Black Holes (PBHs), as those formed in the early universe (M∼10<span>15 </span>g)</p> <p>would persist today, conflicting with gamma-ray background observations [<span>2</span>]. We propose</p> <p>an alternative decay mechanism based on the Selection-Stitch Model (SSM) [<span>3</span>], where the</p> <p>vacuum is modeled as a discrete Face-Centered Cubic (FCC) tensor network. By recognizing</p> <p>the 3D bulk as an isometric holographic projection of a continuous 2D boundary, the vacuum</p> <p>functions as an Isometric Tensor Network (isoTNS) [<span>4</span>]. This mathematical structure retains</p> <p>genuine mechanical properties (domain walls and discrete tension) while simultaneously pre-</p> <p>serving exact Lorentz invariance. Treating the event horizon as a topological vacancy, we</p> <p>apply the Allen-Cahn equation [<span>5</span>] alongside quantum rate theory to derive a "Geometric</p> <p>Evaporation" mode driven by physical lattice tension. We analytically derive a recession</p> <p>velocity of˙</p> <p>R=−(c/2)(l<span>P </span>/R<span>H </span>), yielding a much faster decay law of τ ∝M<span>2</span>. Quantita-</p> <p>tively, a 10<span>15 </span>g PBH evaporates in 0.45 milliseconds via this geometric channel, compared</p> <p>to∼14 billion years via Hawking radiation. A discrete Peierls Locking mechanism with a</p> <p>correlation length of L<span>corr </span>∼1 fm ensures that this rapid channel cleanly eradicates micro-</p> <p>scopic PBHs while exponentially shutting off to leave macroscopic astrophysical black holes</p> <p>perfectly stable.</p> |
| title | Geometric Evaporation: Solving the Primordial Black Hole Constraint via Lattice Tension in an Isometric Holographic Vacuum |
| url | https://doi.org/10.5281/zenodo.18896991 |