On the structure and evolution of a polar crown prominence/filament system

Abstract

Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.

24 pages, 14 figures, Accepted for publication in Solar Physics Journal, Movies can be found at http://www2.mps.mpg.de/data/outgoing/panesar/

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Cited by in corpus (11)

• Magnetic Flux Cancelation as the Origin of Solar Quiet Region Pre-Jet Minifilaments
• Network Jets as the Driver of Counter-Streaming Flows in a Solar Filament/Filament Channel
• Collective Study of Polar Crown Filaments in the Past Four Solar Cycles
• Measuring three-dimensional shapes of stable solar prominences using stereoscopic observations from SDO and STEREO
• Destabilization of a Solar Prominence/Filament Field System by a Series of Eight Homologous Eruptive Flares
• Erupting filaments with large enclosing flux tubes as sources of high-mass 3-part CMEs, and erupting filaments in the absence of enclosing flux tubes as sources of low-mass unstructured CMEs
• Large-Scale Vortex Motion and Multiple Plasmoid Ejection Due to Twisting Prominence Threads and Associated Reconnection
• Velocity Response of the Observed Explosive Events in the Lower Solar Atmosphere: I. Formation of the Flowing Cool Loop System
• Quiet Region Jet by Eruption of Minifilament and Associated Change in Magnetic Flux
• Filigree in the Surroundings of Polar Crown and High-Latitude Filaments
• Eruption of prominence triggered by coronal rain in the solar atmosphere observed by SDO/AIA and Stereo/EUVI