High Energy Physics Under MMA-DMF Framework

The current landscape of fundamental physics is characterized by persistent and correlated anomalies that stress the standard theoretical paradigm. On cosmological scales, the Hubble tension and the S8 discrepancy question the completeness of the ΛCDM model. On galactic and cluster scales, the dark matter hypothesis has not converged to a unique microphysical realization. In high-energy astrophysics, magnetar flares, fast radio bursts (FRBs), neutron-star mass gaps, and possible regular black hole cores expose the limits of a purely dark-matter-based explanation. The modified-gravity framework MMA-DMF (Modified Matter Acceleration – Dark Matter Free) proposes an alternative hypothesis: gravity itself is enriched by a single scalar degree of freedom coupled non-minimally to curvature and matter, governed by a unique fundamental energy scale M ≃ 100 TeV. Dark matter is replaced by geometric screening and blocking mechanisms, and the Standard Model mass spectrum is controlled by discrete “geometric flavour charges”. In this work we construct a coherent high-energy phenomenology of MMA-DMF, focusing on compact objects and extreme electromagnetic fields. We specify the effective action, the trace-dependent screening mechanism, the geometric flavour sector and the regular black hole metric. We then implement and apply a validation pipeline that combines cosmological observables (H0, rs, S8, Pantheon+), cluster- and galaxy-scale tests, magnetar vacuum stability, FRB “Sad Trombone” drifts, neutron-star structure (including a Super-TOV branch) and pulsar glitches. Numerical data products (mass–radius curves, stability curves and parameter JSON files) are used to anchor the analysis. We show that, for the audited Version 72 of the framework, the model simultaneously: (i) resolves the H0 and S8 tensions via a transient Early-X scalar bump; (ii) replaces dark haloes by environment-dependent scalar screening; (iii) regularizes black hole cores into de Sitter regions with finite density set by the M = 100 TeV scale; (iv) keeps the QED sector compatible with precision constraints while altering the Schwinger limit in magnetars; (v) supports a stable Super-TOV neutron-star branch up to M ∼ 2.8 M⊙; and (vi) explains large pulsar glitches in a natural way. We identify concrete observational “smoking guns” of the framework, including scalar breathing modes in magnetar flares, polarization signatures and specific FRB drift patterns. The overall conclusion is that MMA-DMF survives a broad audit of high-energy tests and constitutes a serious candidate for a dark-matter-free explanation of the missing-mass problem.