Steady-state stellar wind characteristics of TOI-700. (a) The 3D stellar wind configuration comprising select magnetic field lines. Contours in the background illustrate stellar wind speed at the equatorial plane (z = 0). The blue isosurface signifies the critical surface beyond which the stellar wind becomes supermagnetosonic (or “superfast”). Black solid lines indicate the orbits of three planets, namely, TOI-700 b, TOI-700 c, and TOI-700 d. (b) Stellar wind dynamic pressure in the equatorial plane normalized by the solar wind dynamic pressure at 1 au. (c) Stellar wind density in the equatorial plane normalized by the solar wind density at 1 au. In panels (b) and (c), the dashed line represents the critical surface location.