This also explains why CMEs and solar flares typically erupt from what are known as the active regions on the Sun where magnetic fields are much stronger on average. The helical magnetic field and the material that it contains may violently expand outwards forming a CME.
The sudden release of energy during this process causes the solar flare and ejects the CME. These lines of force quickly reconnect into a low arcade of loops, leaving a helix of magnetic field unconnected to the rest of the arcade.
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On the Sun, magnetic reconnection may happen on solar arcades-a series of closely occurring loops of magnetic lines of force.
As the Sun's magnetic field lines become more and more twisted, CMEs appear to be a 'valve' to release the magnetic energy being built up, as evidenced by the helical structure of CMEs, that would otherwise renew itself continuously each solar cycle and eventually rip the Sun apart. These magnetic field lines can become twisted in a helical structure, with a 'right-hand twist' or a 'left-hand twist'. Reconnection releases energy stored in the original stressed magnetic fields. In magnetohydrodynamic theory, the sudden rearrangement of magnetic field lines when two oppositely directed magnetic fields are brought together is called "magnetic reconnection". The phenomenon of magnetic reconnection is closely associated with CMEs and solar flares. They are usually observed with a white-light coronagraph. Ĭoronal mass ejections are associated with enormous changes and disturbances in the coronal magnetic field. While the terrestrial effects of solar flares are very fast (limited by the speed of light), CMEs are relatively slow, developing at the Alfvén speed. The ejected material is a magnetized plasma consisting primarily of electrons and protons.
Īrcs rise above an active region on the surface of the Sun.Ĭoronal mass ejections release large quantities of matter and electromagnetic radiation into space above the Sun's surface, either near the corona, or farther into the planetary system, or beyond (interplanetary CME). The largest recorded geomagnetic perturbation, resulting presumably from a CME hitting the Earth's magnetosphere, was the solar storm of 1859 (the Carrington Event), which took down parts of the recently created US telegraph network, starting fires and shocking some telegraph operators. Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days. CMEs most often originate from active regions on the Sun's surface, such as groupings of sunspots associated with frequent flares. Ĭoronal mass ejections are often associated with other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established. The plasma is released into the solar wind, and can be observed in coronagraph imagery. They often follow solar flares and are normally present during a solar prominence eruption. A coronal mass ejection ( CME) is a significant release of plasma and accompanying magnetic field from the solar corona.
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