Magnetic reconnection
![Magnetic Reconnection: This view is a cross-section through four magnetic domains undergoing separator reconnection. Two separatrices (see text) divide space into four magnetic domains with a separator at the center of the figure. Field lines (and associated plasma) flow inward from above and below the separator, reconnect, and spring outward horizontally. A current sheet (as shown) may be present but is not required for reconnection to occur. This process is not well understood: once started, it proceeds many orders of magnitude faster than predicted by standard models.](/Images/godic/202501/25/Reconnection0105.gif")
![A magnetic reconnection event on the sun.](/Images/godic/202501/25/-SDO_Observes_a_Reconnection_Event.ogg0105.jpg")
![The evolution of magnetic reconnection during a solar flare.[1]](/Images/godic/202501/25/-Quad-flare.ogg0105.jpg")
Magnetic reconnection is a physical process in highly conducting plasmas in which the magnetic topology is rearranged and magnetic energy is converted to kinetic energy, thermal energy, and particle acceleration. Magnetic reconnection occurs on timescales intermediate between slow resistive diffusion of the magnetic field and fast Alfvénic timescales.