[PEM17-24] Determination of 3D velocity fields of disappearing and erupting solar filaments using SMART/SDDI at Hida observatory
Keywords:space weather, filament dissapearance, filament eruption
The SDDI (Solar Dynamics Doppler Imager) installed in SMART (Solar Magnetic Activity Research Telescope) in Hida observatory can take the solar chromospheric full-disk dataset with 0.25 Angstrom step between -9 to +9 Angstrom centered at H-alpha line. This means that we can get a spectrum of the H-alpha line for the entire region of the filament. In this study, by applying the Beckers's “cloud model” to the filament observation at 73 wavelengths, we can detect the line of sight velocity up to 400km/s.
We calculated the line of sight velocities of the filament eruption which started at 23:30UT on 2016 August 9. The filament is located at the north east limb of the sun, and ejected to become a CME. We tracked the three-dimensional morphological changes of the filament structure entirely from the pre-ejection stage to the disappearance by checking the dense part in H-alpha and AIA images by eyes. We also confirmed the magnetic structure of the erupted filament by using a magnetogram taken with Solar Dynamic Observatory (SDO) /Helioseismic and Magnetic Imager (HMI). We also compared the activities of filament eruption and CME from the aspect of the time variation of the speed and direction to obtain the detailed evolution of the filament eruption which is useful for the space weather forecast.