Travelling solar wind disturbance coming from the Sun (from right in the video) impacts the induced magnetosphere of Venus in the HYB simulation. The colouring gives the number density of the solar wind protons (1/m^3) on the plane of the interplanetary magnetic field vector and the solar wind velocity vector. The center of the planet is in the center of the video. The plasma is dense in the red regions and tenuous in the blue regions. Time shown on the top of the video is in milliseconds (0.001 s) and the total simulated time (t) is about 700 seconds. The disturbance, a solar wind density enhancement shown as a red "wall", enters into the simulation box at t ~ 300 s and has moved through the entire simulation box by t ~ 410 s. (Animation by R. Jarvinen/FMI).
<a rel="nofollow" class="external text" href="https://www.youtube.com/channel/UC-auXDoJSbYBVrSsI2-NpPg">HYB Code</a>
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<bdo lang="en" dir="ltr"><a href="//commons.wikimedia.org/wiki/Commons:YouTube_files" title="Commons:YouTube files">YouTube</a>: <a rel="nofollow" class="external text" href="https://www.youtube.com/watch?v=gnvAV-OR5Tc"><bdi lang="">Solar storm at Venus in the HYB simulation</bdi></a> – View/save archived versions on <a rel="nofollow" class="external text" href="https://web.archive.org/web/*/https://www.youtube.com/watch?v=gnvAV-OR5Tc">archive.org</a> and <a rel="nofollow" class="external text" href="https://archive.today/https://www.youtube.com/watch?v=gnvAV-OR5Tc">archive.today</a></bdo>