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2026
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| Online Access: | https://doi.org/10.5281/zenodo.19039898 |
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| _version_ | 1866901884255600640 |
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| author | Bashan, Nadav |
| author_facet | Bashan, Nadav |
| contents | <p>Recent data from the Dark Energy Spectroscopic Instrument sharpen the late-time tension with a strictly constant cosmological term when the expansion history is expressed in standard bulk variables.</p> <p>In the present framework, the quantity governing cosmic acceleration is not an effective bulk dark energy density, but the boundary-normalized horizon relation</p> <p>ΛR_H² = π³/15.</p> <p>When this fixed geometric relation is rewritten in bulk form through</p> <p>R_H = c / H,</p> <p>it gives an effective equation of state,</p> <p>w_eff = −1 − 2Ḣ / (3H²).</p> <p>For the flat background</p> <p>Ω_Λ = π³/45,</p> <p>Ω_m = 1 − π³/45,</p> <p>and</p> <p>H²(a) / H₀² = Ω_m a⁻³ + Ω_Λ,</p> <p>this yields</p> <p>w₀ = −π³/45 ≃ −0.6890</p> <p>and</p> <p>w_a = 3Ω_ΛΩ_m ≃ 0.6428.</p> <p>These values do not arise from an additional fit, but follow directly from the fixed horizon normalization under spatial flatness.</p> <p>The DESI signal is thus interpreted not as evidence for a new dark energy fluid, but as the bulk projection of a fixed boundary constraint.</p> <p>Late-time cosmology is thereby governed by boundary geometry, while the apparent bulk evolution is the projected form of a fixed horizon relation.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_19039898 |
| institution | Zenodo |
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| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | The DESI Dark Energy Tension as a Boundary Projection Effect Bashan, Nadav <p>Recent data from the Dark Energy Spectroscopic Instrument sharpen the late-time tension with a strictly constant cosmological term when the expansion history is expressed in standard bulk variables.</p> <p>In the present framework, the quantity governing cosmic acceleration is not an effective bulk dark energy density, but the boundary-normalized horizon relation</p> <p>ΛR_H² = π³/15.</p> <p>When this fixed geometric relation is rewritten in bulk form through</p> <p>R_H = c / H,</p> <p>it gives an effective equation of state,</p> <p>w_eff = −1 − 2Ḣ / (3H²).</p> <p>For the flat background</p> <p>Ω_Λ = π³/45,</p> <p>Ω_m = 1 − π³/45,</p> <p>and</p> <p>H²(a) / H₀² = Ω_m a⁻³ + Ω_Λ,</p> <p>this yields</p> <p>w₀ = −π³/45 ≃ −0.6890</p> <p>and</p> <p>w_a = 3Ω_ΛΩ_m ≃ 0.6428.</p> <p>These values do not arise from an additional fit, but follow directly from the fixed horizon normalization under spatial flatness.</p> <p>The DESI signal is thus interpreted not as evidence for a new dark energy fluid, but as the bulk projection of a fixed boundary constraint.</p> <p>Late-time cosmology is thereby governed by boundary geometry, while the apparent bulk evolution is the projected form of a fixed horizon relation.</p> |
| title | The DESI Dark Energy Tension as a Boundary Projection Effect |
| url | https://doi.org/10.5281/zenodo.19039898 |