Bidirectional Reconnection Outflows in an Active Region

We report on bidirectional coronal reconnection outflows reaching 200 km s−1 as observed in an active region with the Si iv and C ii spectra of the Interface Region Imaging Spectrograph (IRIS). The evolution of the active region with an emerging flux, a failed filament eruption, and a jet is followe...

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Bibliographic Details
Published in:The Astrophysical journal 2019-09, Vol.883 (1), p.52
Main Authors: Ruan, Guiping, Schmieder, Brigitte, Masson, Sophie, Mein, Pierre, Mein, Nicole, Aulanier, Guillaume, Chen, Yao
Format: Article
Language:English
Subjects:
Astrophysics
Blue shift
Corona
Eruptions
Filters
Magnetic fields
Magnetism
Outflow
Physics
radiation: dynamics
Red shift
Sun: activity
Sun: UV radiation
techniques: imaging spectroscopy
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Summary:We report on bidirectional coronal reconnection outflows reaching 200 km s−1 as observed in an active region with the Si iv and C ii spectra of the Interface Region Imaging Spectrograph (IRIS). The evolution of the active region with an emerging flux, a failed filament eruption, and a jet is followed in Solar Dynamical Observatory (SDO)/Atmospheric Imaging Assembly (AIA) filters from 304 to 94 , IRIS slit jaw images, and SDO/Helioseismic and Magnetic Imager movies. The bidirectional outflow reconnection is located at a bright point visible in multiwavelength AIA filters above an arch filament system. This suggests that the reconnection occurs between rising loops above the emergence of magnetic bipoles and the longer, twisted magnetic field lines remnant of the failed filament eruption one hour before. The reconnection occurs continuously in the corona between quasi-parallel magnetic field lines, which is possible in a 3D configuration. The reconnection also triggers a jet with transverse velocities around 60 km s−1. Blueshifts and redshifts along its axis confirm the existence of a twist along the jet, which could have been transferred from the filament flux rope. The jet finally blows up the material of the filament before coming back during the second phase. In the H Dopplergrams provided by the MSDP spectrograph, we see more redshift than blueshift, indicating the return of the jet and filament plasma.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ab3657