Solar wind across the heliosphere
MSWIM2D simulates the solar wind throughout the ecliptic plane using a 2D magnetohydrodynamic model driven by OMNI, MIDL, STEREO, and Solar Orbiter observations at 1 AU. The result is a continuous, self-consistent picture of plasma conditions from Earth's orbit out to 75 AU, covering every planet, every spacecraft, every longitude.
At a glance
Time range
1985 – 2025, updated periodically
Cadence
1 hour
Coverage
Ecliptic plane, all longitudes, 1 – 75 AU
Output variables
Bx By Bz (nT), Ux Uy Uz (km/s), ρ (amu/cm3), Ti (K)
Driven by
OMNI near-Earth solar wind, MIDL merged L1 data, STEREO-A & STEREO-B, Solar Orbiter (propagated to 1 AU)
Version
Current release V2.0.0. The previous site remains available at MSWIM2D.V1.
Why MSWIM2D
Spacecraft beyond 1 AU measure the solar wind only along their own trajectory. MSWIM2D fills in the rest of the ecliptic plane with a physics-based MHD simulation, giving researchers continuous context for any mission in the heliosphere: past, present, or planned.
- 1Full 2D coverage. Every longitude, every radial distance from 1 to 75 AU. Not a 1D slice along the Sun–Earth line, but the full ecliptic plane, with shocks, CIRs, and CMEs propagating self-consistently in two dimensions.
- 2Multi-source input. The inner boundary combines OMNI and MIDL's quality-screened L1 data with off-Sun-Earth-line measurements from STEREO and Solar Orbiter, giving 360° coverage that no single spacecraft can provide.
- 3Any trajectory. Upload any spacecraft trajectory in HGI coordinates, or pick from 13 built-in targets including planets and deep-space missions, and get interpolated conditions in seconds.