Structural features of high-n gravitational eigenstates

This paper extends the theoretical development of a quantized Newtonian-gravity model of gravitational eigenstates based on the application of Schrodinger's equation to the weak regions of deep gravitational wells such as those of galaxies and galactic clusters [1 - 3]. We present quantitative results from the mathematical techniques that were derived to deal with high-n, high-l states, that have interesting astronomical properties, including extremely long lifetimes and low interaction rates with photons and localized particles. Other factors that contribute to the weak-interaction properties of certain eigenstates are the effective wavefunction amplitude, and the spatial oscillation frequency (SOF). It is seen that for the weakest interacting states, the mechanisms preventing transfer to an eigenspectral state mix appropriate to visible particles fall into two categories: 1) the lack of a suitable overlapping state and 2) differences in the SOF and amplitude of the initial and final state.