SDO/AIA observations of a partially erupting prominence

Journal Article · Sun Dec 01 04:00:00 EST 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/778/2/142· OSTI ID:22341934

Tripathi, Durgesh ^[1]; Reeves, Katharine K. ^[2]; Gibson, Sarah E. ^[3]; Srivastava, Abhishek; Joshi, Navin C. ^[4]

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1. Inter-University Centre for Astronomy and Astrophysics, Pune University Campus, Pune 411007 (India)
2. Smithsonian Astrophysical Observatory, 60 Garden Street, MS 58, Cambridge, MA 02138 (United States)
3. High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO 80307-3000 (United States)
4. Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263129 (India)

We report an observation of a partially erupting prominence and its associated dynamical plasma processes based on observations recorded by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. The prominence first went through a slow rise (SR) phase followed by a fast rise (FR) phase. The SR phase began after a couple of small brightenings were seen toward the footpoints. When the prominence had transitioned from SR to FR, it had already become kinked. The prominence shows strong brightening at the central kink location during the start of FR. We interpret this as an internal magnetic reconnection occurring at a vertical current sheet forming between the two legs of the erupting prominence (flux rope). The brightening at the central kink location is seen in all EUV channels of AIA. The contributions of differential emission at higher temperatures are larger compared to that for typical coronal temperatures supporting a reconnection scenario at the central kink location. The plasma above the brightening location is ejected as a hot plasmoid-like structure embedded in a coronal mass ejection, and those below the brightening move down in the form of blobs moving toward the Sun's surface. The unique time resolution of the AIA has allowed these eruptive aspects, including SR-to-FR, kinking, central current sheet formation, plasmoid-like eruption, and filament 'splitting', to be observed in a single event, providing strong and comprehensive evidence in favor of the model of partially erupting flux ropes.

• OSTI ID: 22341934
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 778; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ATMOSPHERES
COMPARATIVE EVALUATIONS
EMISSION
ERUPTION
FILAMENTS
MAGNETIC FIELDS
MAGNETIC RECONNECTION
MASS
PLASMA
SUN
SURFACES
TIME RESOLUTION
ULTRAVIOLET RADIATION