Possible Causes of Dark Matter Distribution in the Early Universe: Based on Quantum Fluctuations

Abstract

Studying the early universe’s formation is key to understanding current cosmic structures, especially dark matter distribution—vital for shaping galaxy clusters, filamentary networks, and voids like KBC voids. Existing theories (Big Bang, inflation, Cold Dark Matter) underpin cosmic evolution but lack a clear link between early dynamics and dark matter’s specific distribution. Drawing on quantum fluctuation theory and observational data (cosmic microwave background/CMB radiation, early galaxy redshift, dark matter halo observations), this paper hypothesizes: In the extremely short period of time (10⁻³⁶–10⁻³² seconds) after the Big Bang, the universe’s exponential expansion stretched microscopic quantum fluctuations to macroscopic scales. These induced spatial density perturbations: higher-density regions, with stronger gravity, attracted baryonic and dark matter, evolving into galaxy clusters/nodes; lower-density areas, lacking strong gravity and depleted of matter by neighbors, formed voids. Quantum fluctuations’ continuity and randomness can explain well the phenomena of dark matter network’s branching and galaxies’ clustered distribution. The hypothesis accounts for major cosmic structures but faces challenges (e.g., quantifying dark matter filament length/branching, verifying “heavy element drag” in curved network regions). Future research should prioritize measuring primordial gravitational waves, high-resolution galaxy structure observations, curved region element analysis, and quantum fluctuation experiments to complement cosmic evolution theories and clarify early dark matter distribution origins.