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The outer solar atmosphere, i.e., the corona and the chromosphere, is repletewith small energy-release events, which are accompanied by transientbrightening and jet-like ejections. These events are considered to be magneticreconnection events in the solar plasma, and their dynamics have been studiedusing recent advanced observations from the Hinode spacecraft and otherobservatories in space and on the ground. These events occur at differentlocations in the solar atmosphere, and vary in their morphology and amount ofthe released energy. The magnetic field configurations of these reconnectionevents are inferred based on observations of magnetic fields at thephotospheric level. Observations suggest that these magnetic configurations canbe classified into two groups. In the first group, two anti-parallel magneticfields reconnect to each other, yielding a 2D emerging flux configuration. Inthe second group, helical or twisted magnetic flux tubes are parallel or at arelative angle to each other. Reconnection can occur only between anti-parallelcomponents of the magnetic flux tubes and may be referred to as componentreconnection. The latter configuration type may be more important for thelarger class of small-scale reconnection events. The two types of magneticconfigurations can be compared to counter-helicity and co-helicityconfigurations, respectively, in laboratory plasma collision experiments.

3D magnetic field configuration of small-scale reconnection events in the solar plasma atmosphere