A stylized flare star sheds charged particles along twisted magnetic loops that arc out of the photosphere and reconnect. Flare power sets the corona's brightness and how hard particles are launched off the surface; CME speed sets their outward velocity once free; magnetic field controls how many loops stay closed (higher field = brighter, denser loop lattice); stellar rotation spins the whole structure so loops sweep past the observer, the way a real active region rotates across the solar disk over days.
- Flare class — a GOES-style label (M / X1 / X2+) derived from flare power, matching the M/X classification used for real solar flares.
- Plasma flux — particles per second crossing the escape radius, i.e. how much of the ejection actually leaves the corona rather than falling back.
- Temperature — flare-heated plasma temperature in megakelvin (MK); real X-class flares reach 10-20+ MK.