Three-dimensional MHD simulation of a recurring eruption within an emerging flux region of the Sun. Magnetic fields are generated within the convective region of our star, and result in sunspot and so-called "active regions" on the solar surface. Eruptions from these regions produce flares and coronal mass ejections, which are related to twisted magnetic flux tubes in the solar atmosphere called "flux ropes". This simulation studies how such structures become eruptively unstable. The visualization shows temperature, from 5600K (black) to 10MK (white), at two different times roughly six minutes apart (left and right sides, respectively). Two subsequent eruptions have collided between these two points in time.
Methods: Lare3D code