Asteroid Magnetization from the Early Solar Wind

**Figure 4.** ([arXiv](http://arxiv.org/abs/2105.08852)) Steady state view of the magnetic field lines draping over the surface of the asteroid (shown in translucent white). The field lines are colored by their strength relative to the incoming solar wind values on a *logscale* (see PDF placeholder image for colorbar) from 0.5 (blue) to 10 (red). The field lines were integrated from points evenly spaced along a line across the bottom boundary (y = -12R, z = 0), as well as points withing a sphere of radius 1.2R centered at the center of the asteroid . This case corresponds to the denser solar wind (ion density 1000 per cc), and a constant magnetic Reynolds' number of 5,000 inside the asteroid.