Self Consistent Modeling of Turbulence Transport with Implications for Cosmic Ray Transport and Modulation

A global solar wind turbulence model is discussed in a simulation domain spanning from 0.2 AU to 100 AU excluding the effect of termination shock at present. The three governing equations which model the turbulence describe fluctuation energy, correlation scale and temperature at every point in the heliosphere. These equations are solved numerically along every radial direction in our simulation domain. The parameters present in these equations are varied along the inner boundary and across the simulation domain. These parameters are magnetic variance, correlation length, plasma temperature, plasma shear, wind speed, strength of pick-up ions, and cross helicity, among others. The simulation results thus obtained are compared with observations. The turbulence model is then combined with a modulation code that integrates Parker's transport equation numerically. This is part of our ongoing effort to integrate turbulence and scattering self consistently and develop an ab initio model of the solar modulation of cosmic rays. Implications for cosmic ray scattering and transport in the outer heliosphere will be discussed in light of recent Voyager observations at 85 AU.