Numerical Modeling of Solar Wind Flow Using Interplanetary Scintillation Data as Boundary Conditions

摘要

Accurate modeling of the plasma flow in the outer heliosphere demands use of realistic boundary conditions that are three-dimensional and time-dependent. We prepare such boundary conditions using solar wind parameters derived from interplanetary scintillation observations and feed them into the Multi-scale Fluid-Kinetic Simulation Suite, which is a package of numerical codes proven to be capable of handling the complex processes occurring in the outer heliosphere characterized by interactions between the solar wind and the partially ionized interstellar medium. We present the simulation results that include comparisons to Voyager measurements across the termination shock and in the inner heliosheath.