Abstract
We analyzed simultaneous EUV images from the Transition Region And Coronal Explorer (TRACE) and Hα and Hβ filtergrams from Huairou Solar Observing Station (HSOS). In active region NOAA 8307, an Hα C5.5 flare occurred near 06:10 UT on 23 August 1998. In this paper, we concentrated on loop–loop interaction, as well as their relationship to the C5.5 flare. We find that while opposite polarity magnetic fields cancelled each other, Hβ bright points appeared, and then the flare occurred. Looking at EUV images, we noticed that a TRACE flare, associated with the C5.5 flare in Hα and Hβ filtergrams, first appeared as patch-shaped structures, then the flare patches expanded to form bright loops. We used a new numerical technique to extrapolate the chromospheric and coronal magnetic field. Magnetic field loops, which linked flare ribbons, were found. It was suggested that loop interaction in the active region was the cause of the TRACE and Hα flare; the magnetic topological structures were clearly demonstrated and the TRACE flare was probably due to the interaction among energetic low-lying and other longer (higher) magnetic loops. Each primary flare kernel, seen from Hα, Hβ filtergrams, and EUV images, was located near the footpoints of several interacting loops.
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Zhang, J., Wang, J. Loop interaction scenario of a trace flare. Solar Physics 196, 377–393 (2000). https://doi.org/10.1023/A:1005272919246
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DOI: https://doi.org/10.1023/A:1005272919246