  A model is presented allowing calculation of energy and matter distribution
in the Universe after expansion from singularity without introduction of
expansion energy. Beginning with Fick's law of diffusion, we solve the Bessel
function for spherical systems during expansion, presuming isotropic matter
distribution in the Hubble flow. This function can be substituted with the
Associated Legendre differential equation and when solved we discover useful
parameters for those of energy and matter densities, diffusion and temperature.
Though we can follow the decline of matter density over spacetime, we cannot
suggest a precise value at singularity. This model may be useful though, as a
starting point for modeling star formation rates, SFR, galaxy formation horizon
lengths and regions devoid of matter where tracing the matter density decline
over time is important.
