Fine-scale Explosive Energy Release at Sites of Prospective Magnetic Flux Cancellation in the Core of the Solar Active Region Observed by Hi-C 2.1, IRIS, and SDO

• Published in: The Astrophysical journal 2019-12, Vol.887 (1), p.56
• Main Authors: Tiwari, Sanjiv K., Panesar, Navdeep K., Moore, Ronald L., Pontieu, Bart De, Winebarger, Amy R., Golub, Leon, Savage, Sabrina L., Rachmeler, Laurel A., Kobayashi, Ken, Testa, Paola, Warren, Harry P., Brooks, David H., Cirtain, Jonathan W., McKenzie, David E., Morton, Richard J., Peter, Hardi, Walsh, Robert W.
• Format: Article
• Language: English
• Subjects: Arches; Astrophysics; Bombs; Brightening; Corona; Fluctuations; Light curve; Line spectra; Magnetic flux; Outflow; Photosphere; Polarity; Solar active region magnetic fields; Solar active regions; Solar activity; Solar activity regions; Solar corona; Solar magnetic flux emergence; Solar photosphere; Solar transition region; Temporal resolution
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ab54c1

The second Hi-C flight (Hi-C 2.1) provided unprecedentedly high spatial and temporal resolution (∼250 km, 4.4 s) coronal EUV images of Fe ix/x emission at 172 of AR 12712 on 2018 May 29, during 18:56:21-19:01:56 UT. Three morphologically different types (I: dot-like; II: loop-like; III: surge/jet-like) of fine-scale sudden-brightening events (tiny microflares) are seen within and at the ends of an arch filament system in the core of the AR. Although type Is (not reported before) resemble IRIS bombs (in size, and brightness with respect to surroundings), our dot-like events are apparently much hotter and shorter in span (70 s). We complement the 5 minute duration Hi-C 2.1 data with SDO/HMI magnetograms, SDO/AIA EUV images, and IRIS UV spectra and slit-jaw images to examine, at the sites of these events, brightenings and flows in the transition region and corona and evolution of magnetic flux in the photosphere. Most, if not all, of the events are seated at sites of opposite-polarity magnetic flux convergence (sometimes driven by adjacent flux emergence), implying likely flux cancellation at the microflare's polarity inversion line. In the IRIS spectra and images, we find confirming evidence of field-aligned outflow from brightenings at the ends of loops of the arch filament system. In types I and II the explosion is confined, while in type III the explosion is ejective and drives jet-like outflow. The light curves from Hi-C, AIA, and IRIS peak nearly simultaneously for many of these events, and none of the events display a systematic cooling sequence as seen in typical coronal flares, suggesting that these tiny brightening events have chromospheric/transition region origin.