Formation of Compact Stars as a Dynamic Process: Cumulative Accumulation of Internal Energy, Surpassing of Equilibrium, and the Limit of Neutronic Stabilization

The properties of high-density matter in neutron stars are commonly described through equations of state in which internal pressure is treated as a local function of density. In particular, models based on the physics of strong interactions indicate that, upon reaching the deconfinement regime, matter develops a positive pressure associated with the liberation of the fundamental degrees of freedom, with energy scales typically located in the interval 0. 1–1 GeV/fm³. However, a purely local description of pressure does not explicitly clarify the structural origin of the stability limit of compact stars. In the absence of a mechanism that modifies the transmission of pressure within the system, this approach in fact leads to configurations in which the stabilization of matter would always remain possible through a continuous increase in density, without a natural instability threshold emerging. In this work we introduce a model in which internal pressure is interpreted as the result of a cumulative process, generated by the transmission of energetic contributions through a layered structure. In this context, the pressure associated with deconfinement acts as the primary physical source, while its propagation through the layers produces a structural gradient that modifies the effective pressure of the system. The system is initially described through an equilibrium condition between internal and external pressure, in which internal pressure acts as a suspension mechanism against gravitational compression. However, the introduction of the cumulative contribution leads to the formation of an energy ridge, which represents the point at which pressure transmission is no longer able to sustain the structure in a stable way. This behavior prevents complete stabilization of the system and naturally introduces a mass threshold beyond which equilibrium can no longer be maintained. Unlike purely local models, the limit thus emerges as a direct consequence of the internal structure and not as a parameter imposed from outside. Through the formulation of the model and the comparison with observational data from high-mass neutron stars, we obtain, at the level of an effective model, a characteristic limit in the interval M ≈ 2. 5 – 3 Mₛun, in agreement with observational constraints and with the characteristic energy scales of deconfinement physics. The model does not replace the complete formalization based on the Tolman-Oppenheimer-Volkoff equation and a microscopic equation of state, but introduces an additional structural mechanism that differentiates the present approach from purely local models: the stability of compact stars is here determined by the interaction between QCD-origin pressure, cumulative accumulation of internal contributions, and gravitational compression, offering an interpretative key for the emergence of the observed mass limit.