Abstract:
We study a quiet-Sun blowout jet which was observed on 2014 May 16 by the instruments on board the Solar Dynamics Observatory (SDO). We find the twin CME as jet-like and bubble-like CMEs simultaneously as observed by LASCO C2 on board the Solar and Heliospheric Observatory (SoHO), and the Solar Terrestrial Relation Observatory (STEREO_A and STEREO_B/COR2). They are, respectively, associated with the eruption of the northern and southern sections of the filament. A circular filament is rooted at the internetwork region at the base of the blowout jet. The collective magnetic cancellation is observed by SDO/Helioseismic and Magnetic Imager (HMI) line-of-sight (LOS) magnetograms at the northern end of the filament, which makes this filament unstable and further makes it to erupt in two different stages. In the first stage, the northern section of the filament is ejected, and causes an evolution of the northern part of the blowout jet. This part of the blowout jet is further extended as a collimated plasma beam to form a jet-like CME. We also observe the plasma blobs at the northern edge of the blowout jet resulting from the Kelvin–Helmholtz instability in its twisted magneto-plasma spire. In the second stage, the southern section of the filament erupts in the form of a deformed/twisted magnetic flux rope which forms the southern part of the blowout jet. This eruption is most likely caused by the eruption of the northern section of the filament, which removes the confined magnetic field of the southern section of the filament. Alternative scenarios may be a magnetic implosion between these magnetic structures confined in a much larger magnetic domain. This eruption of the southern section of the filament further results in a bubble-like CME in the outer corona. © 2019, Springer Nature B.V.
