Twin CME Launched by a Blowout Jet Originated from the Eruption of a Quiet-Sun Mini-filament. (arXiv:1905.02475v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Solanki_R/0/1/0/all/0/1">Ritika Solanki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srivastava_A/0/1/0/all/0/1">Abhishek K. Srivastava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_Y/0/1/0/all/0/1">Yamini K. Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dwivedi_B/0/1/0/all/0/1">Bhola N. Dwivedi</a>
We study a quiet-Sun blowout jet which is observed on 2014 May 16 by the
instruments on board Solar Dynamics Observatory (SDO). We find the twin CME as
jet-like and bubble-like CME simultaneously as observed by LASCO C2 on board
Solar and Heliospheric Observatory (SoHO), 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/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, 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
Kelvin-Helmholtz (K-H) instability in its twisted magneto-plasma spire. In the
second stage, southern section of the filament erupts in form of
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 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 southern section of the filament further results in
the bubble-like CME in the outer corona.
We study a quiet-Sun blowout jet which is observed on 2014 May 16 by the
instruments on board Solar Dynamics Observatory (SDO). We find the twin CME as
jet-like and bubble-like CME simultaneously as observed by LASCO C2 on board
Solar and Heliospheric Observatory (SoHO), 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/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, 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
Kelvin-Helmholtz (K-H) instability in its twisted magneto-plasma spire. In the
second stage, southern section of the filament erupts in form of
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 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 southern section of the filament further results in
the bubble-like CME in the outer corona.
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