Abstract

The persistent discrepancy between luminous matter and galactic dynamics continues to motivate the search for the physical origin of dark matter halos. Conventional cold dark matter (CDM) models successfully reproduce large-scale structure but remain challenged by the absence of direct particle detection and small-scale anomalies such as the core–cusp problem. In this work, we propose a novel theoretical framework in which dark matter halos arise from localized spins within quantum space foam. Space-time is treated as a vibrating continuum at the Planck scale, where fluctuations generate long-lasting spin-like excitations. These spins exhibit curl and divergent energy flux components, with the curl flux forming rotational fields that aggregate to produce halo-scale gravitational effects. The model is tested by applying the curl energy flux formalism to a Milky Way–like galaxy and comparing the derived outcomes with established halo models. Using the Navarro–Frenk–White (NFW) profile as a benchmark, the density distribution ρ(r), enclosed mass M(r), gravitational potential Φ(r), and circular velocity vc(r) are computed. The results reproduce key observational signatures, including the flat rotation curves of spiral galaxies and the asymptotic behavior of halo mass profiles. This approach provides a conceptual bridge between quantum fluctuations of space-time and astrophysical halo phenomena, offering an alternative to particle-based CDM scenarios. While limitations remain—particularly the absence of direct experimental validation, the framework highlights the potential of space-foam dynamics as an emergent origin of galactic halos. Future work will focus on extending the model to diverse mass regimes and identifying testable predictions unique to the spin-based mechanism.

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