Збережено в:
| Автор: | |
|---|---|
| Формат: | Recurso digital |
| Мова: | Англійська |
| Опубліковано: |
Zenodo
2026
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| Предмети: | |
| Онлайн доступ: | https://doi.org/10.5281/zenodo.19780919 |
| Теги: |
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Зміст:
- <p>We derive the time-dependent dark energy equation of state from the T-symmetric cosmological boundary condition, without introducing any new fields, potentials, or degrees of freedom. Structure formation generates Weyl curvature in the bulk, violating the boundary constraint C=0 at a rate proportional to D'=Df. Conformal self-lensing of the boundary's enforcement response by accumulated structure gives an enhancement factor D, yielding total enforcement power P proportional to D^3*f^2.</p><p>The resulting dark energy density rho_DE = sigma_0 * D^3*f^2/a produces the equation of state w(a) = -2/3 - f - (2/3)*d(ln f)/d(ln a), with zero free shape parameters. A CPL fit gives w0=-0.43, wa=-1.66. Against DESI DR2 (w0=-0.42+/-0.21, wa=-1.75+/-0.58), the model achieves chi^2=0.02 compared to chi^2=11.2 for LCDM.</p><p>The model predicts phantom crossing at z=0.50, peak dark energy density at z=0.51, parameter-free locking of w(z) to the independently measurable growth rate f(z), and eventual disappearance of dark energy as structure growth freezes. The coincidence problem is dissolved: dark energy is strongest when and only when structure is forming. The cosmological constant problem is avoided: Lambda_bg=0 exactly from celestial holography, and the observed acceleration is a transient dissipative effect.</p>