Neutron Star Baryogenesis Through Superfluid Vacuum Cavitation

Standard relativistic magnetohydrodynamics attributes the dense, electron-positron (e⁻e⁺) plasma winds surrounding highly magnetized neutron stars (pulsars and magnetars) to vacuum gap spark discharges and mechanical stripping from the stellar crust. However, these models encounter persistent structural challenges in matching the observed localized injection profiles and absolute chemical purity thresholds. This paper introduces a parsimonious alternative framework based on Quantum Superfluid Vacuum Theory (QSVT). We model the space-time vacuum not as an inert metric continuum, but as a physical, highly energetic Bose-Einstein Condensate (BEC) substrate. Due to the extreme spatial compactness of a 1.4 M_ neutron star, the inward vacuum fluid flow accelerates to relativistic velocities (vvac ~ 0.4c). By applying a unified Bernoulli fluid potential, we demonstrate that the localized vacuum pressure drops below the absolute fluid cavitation threshold within a discrete spherical boundary layer (~ 1.75 km wide) suspended immediately above the solid crust. Simultaneously, the extreme magnetic phase-pumping field (B ~ 10¹¹ T) drives localized tangential fluid acceleration past the universal Schwinger limit. This dual gravitational-electrodynamic tension mechanically tears the continuous fluid vacuum open, transforming transient virtual micro-cavitation fluctuations into a permanent, pristine baryonic plasma wind. We present two distinct observational criteria to test this paradigm utilizing current space-based assets: the total absence of Deuterium absorption lines (D/H ≡ 0) within the active plasma shell, and a non-linear Bogoliubov dispersion signature for crossing gravitational sound wiggles.