Spectral Observations of the Eruption of a Filament

• Published in: Astronomy reports 2019-07, Vol.63 (7), p.608-617
• Main Authors: Mashnich, G. P., Kiselev, A. V.
• Format: Article
• Language: English
• Subjects: Acceleration; Ascent; Astronomy; Coronas; Emission analysis; Emissions; Magnetic fields; Magnetic flux; Observations and Techniques; Physics; Physics and Astronomy; Rupturing; Vertical oscillations
• ISSN: 1063-7729; 1562-6881
• DOI: 10.1134/S1063772919070060

Results of studies of motions in a filament during its slow ascent and eruption based on spectral observations obtained at the Sayan Solar Observatory are presented. SDO/HMI data on the longitudinal magnetic field and SDO/AIA images in the EUV are also considered. Short-period (∼5 min) vertical oscillations of the filament as a whole were detected during its ascent. An acceleration of the rise of the filament was accompanied by the rupture of an orthogonal loop above the filament, which was observed in 193 A EUV images obtained with SDO/AIA over a long time preceding the event. Two hours before the partial eruption of the filament, SDO/HMI data indicate an increase in the magnetic flux by 2 × 10 19 Mx at the footpoints of the loop. The emission from the loop rupture piont propagated toward the east and west along a neutral line, and brightenings were observed at the boundaries of the filament channel. Emission loops were visible in all SDO/AIA channels, testifying to strong heating of the filament plasma. During the rapid phase of the eruption, the filament moved with an acceleration ∼21 m/s 2 . H α images show the filament splitting into fragments parallel to its axis during the eruption. The results of these studies of the eruption of the filament are in agreement with other results in the literature, and are supplemented by new observational facts. Vertical oscillations (∼5 min) of the filament as a whole are observed before the ascent phase. During the ascent phase, an interaction of the filament with a higher-lying coronal loop is observed.