A Relativistic Radiative Hydrodynamic Framework for the Nuclear Impact Hypothesis: Implications for Proto-Stellar Ignition and Planetary Ejection

This manuscript presents a relativistic radiative hydrodynamic framework for the Nuclear Impact Hypothesis. The hypothesis proposes that a hypervelocity nuclear aggregate impactor (v₀ ≳ 10³ km s⁻¹) could trigger proto-solar ignition and eject nascent planetary embryos via asymmetric magnetocentrifugal thrust in a radiation-dominated proto-stellar environment. The model combines Poisson's equation for gravitational potentials, special relativistic momentum conservation, Lorentz forces in magnetized plasmas, three-temperature radiation hydrodynamics, and relativistic Rankine-Hugoniot shock relations, applicable to various stellar configurations. Simulations employ high-resolution cubic interpolation of Standard Solar Model (SSM) profiles constrained by helioseismology (deviations ≲ 8%). These indicate penetration depths δ ≈ 0.05 R⊙ before electromagnetic disassembly and ablation-mediated fragmentation in neutral proto-stellar cores, achieved through refined modeling of relativistic drag and disassembly criteria. The ejection mechanism involves magnetocentrifugal thrust a_thrust = ω² r (B² / 4π ρ) ≳ 10⁻³ c² / R⊙, driven by proto-stellar rotation and magnetism, leading to escape from r₀ = 0.1 R⊙ at velocities v∞ ∼ 40 km s⁻¹. These velocities align with orbital circularization and radiative equilibration timescales in typical systems. Variance-based global Sobol sensitivity analysis (N=2048) highlights the dominance of initial velocity (S_{v₀}=0.65) and thrust (S_{a_thrust}=0.58), with second-order interactions V_{ij} ≈ 0.05. Bayesian propagation gives μ_δ = 0.048 ± 0.012 R⊙. Falsifiability relies on expected Gaia DR4 transients and meteoritic isotopic disequilibria. Grounded in solar wind plasma diagnostics [kasper2016sweap] and relativistic merger hydrodynamics [hu2024energetic, lee2025aic], the framework predicts shock-induced thermonuclear ignition (Ė_diss ∼ 10²² erg cm⁻³ s⁻¹) and density-selective embryo expulsion (ρ > 10 g cm⁻³). It offers insights into Solar System formation and resilience for interstellar probes.