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.

Interpolate along a trajectory

At a glance

Time range

1985 – 2025

1-hour cadence

Updated periodically

Output variables

B_x, B_y, B_z (nT)

U_x, U_y, U_z (km/s)

ρ (amu/cm³), T_i (K)

Driven by

OMNI near-Earth solar wind

MIDL merged L1 data

STEREO-A & STEREO-B

Solar Orbiter (propagated to 1 AU)

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.

Full 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.

Multi-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.

Any 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.

Learn more about the model