Morphology of the flare-productive active region NOAA 9087
Heading:
| 1Chornogor, SN, 1Kondrashova, NN 1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine |
| Kinemat. fiz. nebesnyh tel (Online) 2020, 36(3):69-90 |
| https://doi.org/10.15407/kfnt2020.03.069 |
| Start Page: Solar Physics |
| Language: Ukrainian |
Abstract: Evolution and morphological properties of the active region NOAA 9087 have been analyzed using combination of data from space and ground-based observatories. The hard X-ray (HXR) and soft X-ray (SXR) data were obtained at the Yohkoh Telescopes (HXT and SXT) and Geostationary Operational Environmental Satellite (GOES). The full-disk magnetograms and EUV-images were provided by the Solar and Heliospheric Observatory (SOHO) Michelson Doppler Imager (MDI) and Extreme ultraviolet Imaging Telescope (EIT). We used the -filtergrams from the Meudon spectroheliograph and white light images of Big Bear Solar Observatory (BBSO). Data on the radio emission flux at a frequency of 2.69 GHz was taken from the database of the World Data Center of the Learmonth Observatory (Australia). Active region (AR) studied was observed on the solar disk from 15th to 27th of July, 2000 and showed a complex multipolar magnetic field configuration. The high flare and surge activity was observed in the active region. According to Solar Geophysical Data (SGD) the 3N/M6.4 a long duration two-ribbon flare occurred 19 July 2000 and lasted 2.5 hours. The flare energy was released sequentially in different places of the AR. All the data show continuously evolving SXR, EUV and features during the flare. The HXR and the type III radio bursts were observed at the flare initial phase. A HXR coronal source was located along magnetic polarity inversion line of the active region. EUV loop structures show the observational evidence of a magnetic reconnection during the main phase of the flare. Postflare loops were observed in the 19.5 nm passband at the gradual phase as a manifestation of the EUV late phase. These extended loops connect the sites of primary and secondary of flare energy sources. An additional mechanism of energy transfer and heating existed in the main phase of the flare. |
| Keywords: active regions, magnetic reconnections, multi-wavelength observations, solar flares, Sun |
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