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On the Sun, Doppler shifts of bidirectional outflows from themagnetic-reconnection site have been found only in confined regions throughspectroscopic observations. Without spatially resolved spectroscopicobservations across an extended region, the distribution of reconnection andits outflows in the solar atmosphere cannot be made clear. Magneticreconnection is thought to cause the splitting of filament structures, butunambiguous evidence has been elusive. Here we report spectroscopic and imaginganalysis of a magnetic-reconnection event on the Sun, using high-resolutiondata from the Interface Region Imaging Spectrograph and the Solar DynamicsObservatory. Our findings reveal that the reconnection region extends to anunprecedented length of no less than 14,000 km. The reconnection splits afilament structure into two branches, and the upper branch erupts eventually.Doppler shifts indicate clear bidirectional outflows of ~100 km/s, whichdecelerate beyond the reconnection site. Differential-emission-measure analysisreveals that in the reconnection region the temperature reaches over 10 MK andthe thermal energy is much larger than the kinetic energy. This Letter providesdefinite spectroscopic evidence for the splitting of a solar filament bymagnetic reconnection in an extended region.

Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure