IndisputableMonolith.Nuclear.NuclearForceStructure
NuclearForceStructure asserts that effective nuclear-force coefficients derived from the phi-ladder are positive. Nuclear physicists extending binding-energy models to stability and equation-of-state calculations would cite it to fix the signs of the volume, surface, Coulomb, and asymmetry terms. The module imports the BindingEnergy ledger and factors the positivity claims into four sibling lemmas.
claimThe nuclear force structure yields positive coefficients: volume term $a_v > 0$, surface term $a_s > 0$, Coulomb term $a_c > 0$, and asymmetry term $a_a > 0$, where each coefficient appears in the semi-empirical binding-energy expression obtained from the phi-ladder.
background
Upstream BindingEnergy derives nuclear binding energies from the phi-ladder, confirming the seven magic numbers as eight-tick consequences and addressing question Q16 on whether binding energies follow from the Recognition framework. NuclearForceStructure sits immediately after that ledger and extracts the sign constraints on the effective force coefficients. The module therefore supplies the structural positivity needed before any numerical fitting or stability analysis can proceed.
proof idea
This is a definition module, no proofs. It aggregates four sibling lemmas (nuclear_force_implies_volume_pos, nuclear_force_implies_surface_pos, nuclear_force_implies_coulomb_pos, nuclear_force_implies_asymmetry_pos) that each apply the binding-energy ledger to a single coefficient.
why it matters in Recognition Science
The module feeds IslandOfStabilityStructure and NeutronStarEOSStructure, supplying the positivity constraints those downstream modules require. It thereby closes the structural step that links the phi-ladder binding energies to concrete nuclear-force signs in the Recognition framework.
scope and limits
- Does not derive numerical values for the coefficients.
- Does not address the full semi-empirical mass formula.
- Does not treat quantum corrections or shell effects.
- Does not extend to neutron-star equations of state.