Astrophysical Spectra ⁰ High‑Energy Mode Behavior A. 9

Add‑On A.9 extends the equilibrium‑mode electron framework into stellar, nebular, magnetized, and relativistic environments, showing that astrophysical spectra and high‑energy radiative behavior arise directly from the same structural invariants that govern spectroscopy, angular geometry, transition symmetry, multi‑electron compatibility, ionization thresholds, bonding geometry, scattering deformation, and collective plasma behavior. Radiative transitions, forbidden‑line activation, ionization structure, line broadening, polarization signatures, resonance behavior, and high‑energy spectral deformation are shown to emerge from polarity restoration, angular‑radial coupling, stability‑margin dynamics, phase‑twist symmetry, and radial‑mode compression. A.9 demonstrates that line formation in astrophysical systems reflects stability‑regulated transition structure inherited from A.3 and A.5, while forbidden‑line activation and nebular diagnostics arise from coherence‑limit behavior and stability‑margin geometry. Non‑Saha ionization patterns follow from stability‑regulated mode decoupling, extending the ionization operator of A.5 and the collective‑mode dynamics of A.8 into low‑density and high‑field regimes. High‑energy environments—accretion flows, shocks, jets, and magnetospheres—drive radial‑mode compression and angular collapse, reproducing the high‑momentum scattering behavior of A.7 at astrophysical scales. Phase‑twist symmetry produces polarization‑dependent emissivity, helicity‑dependent absorption, and anisotropic radiative transfer in magnetized plasmas. The resulting formulation provides a unified structural mechanism for astrophysical spectra and high‑energy radiative behavior across stellar atmospheres, nebulae, magnetospheres, shocks, jets, and relativistic plasmas. A.9 completes the radiative and high‑energy layer of the Version 1.0 equilibrium‑mode framework, linking atomic‑scale invariants to astrophysical and extreme‑field behavior.