Siamese Universes v1.0 — Effective QGP → CFL/BEC → LQC Bounce with Guardrails

This repository contains the official final version (v1.0) of the manuscript:

📄 Siamese_Universes_v1.0_Final.pdf
Authors: CosmicThinker & ChatGPT5
Date: Oct 04, 2025

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Abstract

We present a refined effective framework in which matter inside black holes undergoes a sequence of phases — quark–gluon plasma (QGP), color–flavor–locked (CFL) / Bose–Einstein condensation (BEC), and a loop quantum cosmology (LQC)–type bounce — culminating in nonsingular “Siamese” universes. The model includes explicit guardrails: mesoscopic validity (R ≫ ξ ~ 1/Δ), curved-GL perturbative treatment of σ(R), compact Israel–Darmois junctions, flat-prior parameter scans (≈10% bands), and a holographically guided dissipation proxy with C ∈ [0.5, 2]. Synthetic estimates include Tolman corrections O(1–5%) in Δt/H, ~3% reduction of σ at R/ξ=20, and ~15% damping in $\dot{H}(0)$ for C≈1.5, while preserving a robust bounce. A roadmap toward Einstein Toolkit (ETK) viscous GR-hydro simulations is outlined.

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Repository Contents

• Siamese_Universes_v1.0_Final.pdf — main paper (final version, Oct 2025).
• figs/ — synthetic figures:
  • Fig_A1.png: Dual softening (baseline vs bag+gap proxy with ±10% prior band).
  • Fig_B1.png: Tolman perturbative shifts (1–5%) in Δt/H vs curvature scale R/ξ.
  • Fig_C1.png: Damping spread (~10–20%) vs dissipation proxy C.
• (Optional, upcoming): Python scripts to regenerate figures.

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Parameter Priors (summary)

Parameter	Symbol	Range / Prior	Notes
Tolman factor	δ_T	1–5%	Perturbative shift in Δt/H
Gap strength	Δ	lit.-guided	Enters σ₀ ~ c_σ μ²Δ
Dissipation proxy	C	[0.5, 2]	Order unity (holography-inspired)
Sound speed (CFL)	c_s²	0.15 ± 0.02	Effective soft phase

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Roadmap

• Phase I: Mesoscopic scans + RK45 toy evolution.
• Phase II: Post-processing CLASS/ETK outputs with effective softening.
• Phase III: Einstein Toolkit (2025 release) viscous GR-hydro, slow-rotation Kerr interiors.

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Honest Statement

This is an effective scoped toy model. Proxies (Tolman, curved-GL O(λ), dissipation C) are used to quantify trends, not to claim ab initio microphysics near black hole horizons.
All numerical values in the figures are synthetic illustrations only; they should be replaced by calibrated ETK outputs in future simulations.

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Citation

If you use or reference this work, please cite as:

License

This repository is released under the MIT License (see LICENSE if present).