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magnetic reconnection
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The other is magnetic heating, in which magnetic energy is continuously built up by photospheric motion and released through magnetic reconnection in the form of large solar flares and myriad similar but smaller events—nanoflares.
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These twisted magnetic flux tubes, technically known as flux transfer events, form open windows in the planet's magnetic shield through which the solar wind may enter and directly impact Mercury's surface via magnetic reconnection This also occurs in Earth's magnetic field.
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The average temperature of the corona and solar wind is about 1,000,000–2,000,000 K; however, in the hottest regions it is 8,000,000–20,000,000 K. Although no complete theory yet exists to account for the temperature of the corona, at least some of its heat is known to be from magnetic reconnection.
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The reconnection events are analogues to the magnetic substorms in the Earth's magnetosphere.
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When flux tubes loaded with the cold Ionian plasma reach the outer magnetosphere, they go through a reconnection process, which separates the magnetic field from the plasma.
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An extensive analysis of the Cluster results has now shown that the region was experiencing a turbulent event known as 'magnetic reconnection'.
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Terms such as Lorentz force, Gyro movement (gyro bevegelser), ExB-drift, Chapman layers, Hall and Pedersen currents, ring currents, electrojet, magnetic Reynolds number and magnetic reconnection should be known.
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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.
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Philippe Escoubet, ESA's Cluster Project Scientist, comments, "Thanks to Cluster's observations scientists can directly and firmly link for the first time a dayside proton auroral spot and a magnetic reconnection event."
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It is thought that the energy necessary to heat the corona is provided by turbulent motion in the convection zone below the photosphere, and two main mechanisms have been proposed to explain coronal heating.[89] The first is wave heating, in which sound, gravitational or magnetohydrodynamic waves are produced by turbulence in the convection zone.[89] These waves travel upward and dissipate in the corona, depositing their energy in the ambient matter in the form of heat.[146] The other is magnetic heating, in which magnetic energy is continuously built up by photospheric motion and released through magnetic reconnection in the form of large solar flares and myriad similar but smaller events—nanoflares.[147]
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The reconnection processes may correspond to the global reconfiguration events also observed by the Galileo probe, which occurred regularly every 2–3 days.[35] The reconfiguration events usually included rapid and chaotic variation of the magnetic field strength and direction, as well as abrupt changes in the motion of the plasma, which often stopped co-rotating and began flowing outward.
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