Development of a solar circular flare М6.4 according to observations in the Нα line
Heading:
| 1Chornogor, SN, 1Kondrashova, NN 1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine |
| Kinemat. fiz. nebesnyh tel (Online) 2021, 37(2):41-56 |
| https://doi.org/10.15407/kfnt2021.02.041 |
| Start Page: Solar Physics |
| Language: Ukrainian |
Abstract: The development of the 3N / M6.4 flare on July 19, 2000 in the active region of NOAA 9087 was studied based on the analysis of its images in the Нα line.Нα -filtergrams obtained at the Medon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. The flare 3N/M6.4 class began with the appearance of two bright kernels near a large spot. A few minutes later flare kernels appeared in the central part of the active region, where a coronal source of hard X-ray radiation was identified. The flare lasted 2.5 hours. Its energy was released sequentially in different places of the active region. The flare kernels were located along the polarity inversion line at the boundaries of the chromospheric cells. Flare ribbons had a circular shape. An assumption is made about a magnetic topology of the spine-fan type containing null point. In this case, flare ribbons are the intersections of the fan quasi-separatrix layer with the lower atmosphere. The successive appearance of flare kernels may indicate slipping magnetic reconnection in the flare under study. In the Нα-images in the main phase of the flare, there are reconnecting loops in the eastern part of the active region, which are clearly visible in the ultraviolet wavelength range. |
| Keywords: activity, chromosphere, magnetic reconnections, solar flares, Sun |
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