PMO OpenIR  > 太阳活动的多波段观测研究团组
MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12
Su, Yingna1,2; van Ballegooijen, Adriaan2; McCauley, Patrick2; Ji, Haisheng1; Reeves, Katharine K.2; DeLuca, Edward E.2
2015-07-10
Source PublicationASTROPHYSICAL JOURNAL
Volume807Issue:2Pages:144
AbstractWe present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA; end-on view) and displays a quasi-vertical thread structure. A bright U-shaped or horn-like structure is observed surrounding the upper portion of the prominence at 171 angstrom before the eruption and becomes more prominent during the eruption. The disk view of STEREOB shows that this long prominence is composed of a series of vertical threads and displays a half-loop-like structure during the eruption. We focus on the magnetic support of the prominence vertical threads by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO_B. We also construct a series of magnetic field models (sheared arcade model, twisted flux rope model, and unstable model with hyperbolic flux tube). Various observational characteristics appear to be in favor of the twisted flux rope model. We find that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast-rise phase, and signatures of reconnection (posteruption arcade, new U-shaped structure, rising blobs) appear about one hour later. During the eruption, AIA observes dark ribbons seen in absorption at 171 angstrom corresponding to the bright ribbons shown at 304 angstrom, which might be caused by the erupting filament material falling back along the newly reconfigured magnetic fields. Brightenings at the inner edge of the erupting prominence arcade are also observed in all AIA EUV channels, which might be caused by the heating due to energy released from reconnection below the rising prominence.
KeywordSun: Activity Sun: Corona Sun: Coronal Mass Ejections (Cmes) Sun: Filaments Prominences Sun: Magnetic Fields
Subject Area天文和天体物理
WOS HeadingsScience & Technology ; Physical Sciences
DOI10.1088/0004-637X/807/2/144
WOS KeywordCORONAL MASS EJECTIONS ; FLUX ROPES ; RECONNECTION OUTFLOWS ; ACTIVE REGIONS ; CURRENT SHEET ; FILAMENT ; FLARES ; FIELD ; MODEL ; ONSET
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000358967000030
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Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/14914
Collection太阳活动的多波段观测研究团组
Affiliation1.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China
2.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Recommended Citation
GB/T 7714
Su, Yingna,van Ballegooijen, Adriaan,McCauley, Patrick,et al. MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12[J]. ASTROPHYSICAL JOURNAL,2015,807(2):144.
APA Su, Yingna,van Ballegooijen, Adriaan,McCauley, Patrick,Ji, Haisheng,Reeves, Katharine K.,&DeLuca, Edward E..(2015).MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12.ASTROPHYSICAL JOURNAL,807(2),144.
MLA Su, Yingna,et al."MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12".ASTROPHYSICAL JOURNAL 807.2(2015):144.
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