• Intensely magnetized regions around and above sunspot pairs

• Constantly alter their magnetic configuration during their weak to multiple month long existence

• Their concentration of magnetic field lines trap electrically charged particle

• Bright ultraviolet and X-ray radiation are emitted by the hot, electrified gas

• The magnetic field lines of an active region can get very twisted into a state of high energy

• Magnetic field lines can reconnect to a less twisted states of lower energy

• Upon this reconnection is a sudden release of energy...      a solar flare

This image of Active Region 8210 shows the magnetic contours on the photosphere with 3D magnetic field lines connecting positive polarity (red) to negative polarity (blue).