Solar wind flow in the heliosheath due to latitudinal and time variations over the solar cycle

Recent observations by Voyager 2 in the heliosheath showed strong variations of the solar wind density, velocity and temperature. Magnetic field fluctuates considerably as observed on both Voyager 1 and 2. Anomalous and galactic cosmic rays also present large fluctuations of intensity. Spatial variations and temporal effects in the solar wind due to solar cycle attribute to the observed fluctuations. In this work we aim to explore effects of realistic solar cycle on the 3D solar wind flow in the outer heliosphere. We use time and latitudinal variations of the solar wind density and velocity over two last solar cycles as the boundary conditions in a 3D MHD multi-fluid model of the interaction between the solar wind and interstellar medium based on BATSRUS code. These realistic boundary conditions at 1 AU for the plasma were obtained on the base of the measurements of Ly-alpha intensities on SOHO/SWAN and interplanetary scintillations data (IPS). In our simulation a numerical spatial grid is highly refined along the Voyager 2 trajectory in order to capture disturbances propagating in the solar wind and compare the model with the observations. To validate the model and used boundary conditions we compare our results with Voyager 2 plasma data. In particular we focus on the time-dependent plasma flow in the heliosheath.