Contemporary astrophysics models mass loss prior to a supernova explosion primarily through the phenomenological hydrodynamics of hot gases and radiation-driven stellar winds. However, these models fail to causally explain exact mass cuts during collapse or the extreme asymmetry of mass ejections. This paper applies the Hydro-Elastic Model (HEM) to the mechanics of massive star collapse. The defining framework is a 4-dimensional continuum, where we demonstrate that the shedding of outer layers is a strictly deterministic phase transition. It occurs the moment the centrifugal tensile stress within the 3D membrane exceeds the local compressive pressure and reaches the topological yield strength of the matter nodes themselves (Kₚ 3. 0 10^34 Pa). The subsequent topological decomposition (smoothing) of the boundary layer releases locked phase area, generating a massive bidirectional shock wave within the 3D membrane. The conservation of energy during this implosion and explosion exactly dictates the final fate of the star (White Dwarf, Neutron Star, or Black Hole). We analytically derive and numerically validate the exact fracture radius, calculate the mass of the remnant central mass and the ejected envelope, as well as the escape velocity of the catapulted matter. This communication is based on the comprehensive theoretical framework 'The Universe as a Hydro-Elastic 4D Mechanism' (Archived at Zenodo: DOI 10. 5281/zenodo. 19616545).
Tomáš Novotný (2026) studied this question.