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Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
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Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
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Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail

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Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail
Journal Article

Cassini in situ observations of long-duration magnetic reconnection in Saturn’s magnetotail

2016
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Overview
Cassini’s encounter with Saturn’s magnetotail — the long magnetosphere region stretching into space — has revealed that plasma exits the magnetosphere through long-duration magnetic reconnection, which ejects ten times more mass than estimated. Magnetic reconnection is a fundamental process in solar system and astrophysical plasmas, through which stored magnetic energy associated with current sheets is converted into thermal, kinetic and wave energy 1 , 2 , 3 , 4 . Magnetic reconnection is also thought to be a key process involved in shedding internally produced plasma from the giant magnetospheres at Jupiter and Saturn through topological reconfiguration of the magnetic field 5 , 6 . The region where magnetic fields reconnect is known as the diffusion region and in this letter we report on the first encounter of the Cassini spacecraft with a diffusion region in Saturn’s magnetotail. The data also show evidence of magnetic reconnection over a period of 19 h revealing that reconnection can, in fact, act for prolonged intervals in a rapidly rotating magnetosphere. We show that reconnection can be a significant pathway for internal plasma loss at Saturn 6 . This counters the view of reconnection as a transient method of internal plasma loss at Saturn 5 , 7 . These results, although directly relating to the magnetosphere of Saturn, have applications in the understanding of other rapidly rotating magnetospheres, including that of Jupiter and other astrophysical bodies.