Solar wind prediction for Uranus from 1972 to 2020

1. Model We use a 3-D magnetohydrodynamic model that predicts solar wind conditions between 1 and 80 AU using time-dependent boundary conditions implemented in the adaptive mesh refinement framework of Multi-scale Fluid-kinetic Simulation Suite (MS-FLUKSS), which is a numerical toolkit designed primarily for modeling flows of partially ionized plasma (Pogorelov et al. 2014, 2017, 2021; Pogorelov 2023). Simulation domain: 1-80 AUSimulation grid: 1,024 x 128 x 128 (r, phi, theta)Approximate grid size: dr = 0.05 - 0.1 AU, dphi = 2.8 deg, dtheta = 1.4 deg At 1 AU, the solar wind boundary conditions are derived from OMNI data at low latitudes and fit to Ulysses data at middle to high latitudes (e.g., Kim et al. 2016, 2017; Lamy et al. 2017, 2018; Collet et al. 2025; Zirnstein et al. 2022, 2024). At 80 AU, the interstellar neutral hydrogen atom parameters are: Number density = 0.127 cm^3 (Swaczyna et al. 2020, 2025)Flow speed = 22 km/s (Lellement et al. 2005)Temperature = 10,000 K. 2. Data (Kim et al. 2022) The simulation data file ("Uranus_1972-2020_MS-FLUKSS.dat") consists of a header and 26 columns of numeric values in the following order: Time (fractional year) Heliocentric Distance (au) MS-FLUKSS longitude MS-FLUKSS latitude Total proton number density (cm^-3) Solar wind Vr (km/s) Solar wind Vphi (km/s) Solar wind Vtheta (km/s) Thermal pressure of solar wind and interstellar pickup ion mixture (picodyne/cm^2) Br (nT) Bphi (nT) Btheta (nT) Turbulence energy (km^2) Normalized turbulence cross helicity Turbulence correlation length (au) Pickup proton number density (cm^-3) Pickup proton thermal pressure (picodybe/cm^2) Interstellar hydrogen atom number density (cm^-3) Interstellar hydrogen Vr (km/s) Interstellar hydrogen Vphi (km/s) Interstellar hydrogen Vtheta (km/s) Interstellar hydrogen atom thermal pressure (picodyne/cm^2) Level set for heliospheric current sheet tracking Temperature of the proton mixture (K) Interplanetary magnetic field strength (nT) Total proton dynamic pressure (nPa) 3. Figure The figure shows the simulated interplanetary magnetic field, solar wind dynamic pressure, radial velocity, and total proton number density at Uranus from 1972 to 2020.