2020/06/07 by Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore +1 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Channel (broadcasting) #Earthquake Detection and Analysis #Flux (metallurgy) #Ionosphere and magnetosphere dynamics #Jet (fluid) #Magnetic field #Magnetic flux #Protein filament #Solar and Space Plasma Dynamics #Solar observatory #Spectrograph #astro-ph.SR
paper · pdf · doi:10.3847/2041-8213/ab9ac1
12 pages, 7 figures and 1 table; Accepted for publication in ApJ Letters
arxiv created 2020/06/07 · openalex created_date 2020/06/12 · openalex publication_date 2020/06/25 · arxiv updated 2020/07/01 · openalex updated_date 2026/08/06
Abstract Counter-streaming flows in a small (100″ long) solar filament/filament channel are directly observed in high-resolution Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) extreme-ultraviolet (EUV) images of a region of enhanced magnetic network. We combine images from SDO/AIA, SDO/Helioseismic and Magnetic Imager (HMI), and the Interface Region Imaging Spectrograph (IRIS) to investigate the driving mechanism of these flows. We find that: (i) counter-streaming flows are present along adjacent filament/filament channel threads for ∼2 hr, (ii) both ends of the filament/filament channel are rooted at the edges of magnetic network flux lanes along which there are impinging fine-scale opposite-polarity flux patches, (iii) recurrent small-scale jets (known as network jets ) occur at the edges of the magnetic network flux lanes at the ends of the filament/filament channel, (iv) the recurrent network jet eruptions clearly drive the counter-streaming flows along threads of the filament/filament channel, (v) some of the network jets appear to stem from sites of flux cancelation, between network flux and merging opposite-polarity flux, and (vi) some show brightening at their bases, analogous to the base brightening in coronal jets. The average speed of the counter-streaming flows along the filament/filament channel threads is 70 km s −1 . The average widths of the AIA filament/filament channel and the H α filament are 4″ and 2.″5, respectively, consistent with the earlier findings that filaments in EUV images are wider than in H α images. Thus, our observations show that the continually repeated counter-streaming flows come from network jets, and these driving network jet eruptions are possibly prepared and triggered by magnetic flux cancelation.