JpGU-AGU Joint Meeting 2017

Presentation information

[EE] Poster

P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM18] [EE] Origin of Earth-affecting Coronal Mass Ejections

Wed. May 24, 2017 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall HALL7)

convener:No? Lugaz(University of New Hampshire Main Campus), Kanya Kusano(Institute for Space-Earth Environmental Research, Nagoya University), Neel P Savani(NASA GSFC / University of Maryland Baltimore County), Ayumi Asai(Astronomical Observatory, Kyoto University)

[PEM18-P02] Increase in the amplitude of line-of-sight velocity of the small scale motion as the precursor of filament eruptions

*Daikichi SEKI1, Hiroaki Isobe1, Kenichi Otsuji2, Kumi Hirose2 (1.Graduate School of Advanced Integrated Studies in Human Survivability, Kyoto University, 2.Kwasan and Hida Observatories, Kyoto University)

Keywords:prominence, filament activation, line-of-sight velocity

Filaments, the dense cooler plasmas in the solar corona, often become unstable and erupt into the interplanetary space as coronal mass ejections (CMEs). The CMEs may cause geomagnetic storms that result in various societal and economical impacts such as blackouts and satellite anomalies, so that it is important to predict when filament eruptions will occur. From the space weather point of view, monitoring filaments as the progenitor of CMEs has a following advantage that we can monitor not only flares from active regions but also the eruptions from quiet regions that may also cause severe geomagnetic storms. The aim of this study is to investigate the characteristics of eruptive filaments that can be used as the precursor of eruptions.

For this purpose, we analyzed the solar full disk images captured by Solar Dynamics Doppler Imager(SDDI) installed on Solar Magnetic Activity Research Telescope(SMART) at Hida Obser- vatory, Kyoto University. SDDI can obtain solar full disk images in 73 wavelengths between Hα center-9A and Hα center+9A per 0.25A with the time resolution of about 15 seconds. Therefore this instrument can observe unprecedented detailed line-of-sight velocities of filaments. Focusing on this feature, we calculated the filament’s line-of sight velocities for each pixel of the images by utilizing Beckers’ cloud model from before the eruption, and making histograms of the number of pixels and line-of-sight velocities for each pixel. As the result, we found an increase in the amplitude of line-of-sight velocity of the small scale motions in the filament about one hour before the onset of the eruption, i.e. the FWHM of the fitted gaussian increased. This result can be possibly used as the precursor of filament eruptions