Filament eruption on 2010 October 21 from three viewpoints
arXiv:1306.0679 · doi:10.1088/0004-637X/773/1/10
Abstract
A filament eruption on 2010 October 21 observed from three different viewpoints by the Solar Terrestrial Relations Observatory (STEREO) and the Solar Dynamic Observatory (SDO) is analyzed with invoking also data from the Solar and Heliospheric Observatory (SOHO) and the Kanzelhoehe Solar Observatory. The position of the filament just before the eruption at the central meridian not far from the center of the solar disk was favorable for photospheric magnetic field measurements in the area below the filament. Because of this, we were able to calculate with high precision the distribution of the coronal potential magnetic field near the filament. We found that the filament began to erupt when it approached the height in the corona where the magnetic field decay index was greater than one. We determined also that during the initial stage of the eruption the filament moved along the magnetic neutral surface.
Accepted for publication in ApJ
References in corpus (4)
- Numerical simulations of fast and slow coronal mass ejections
- Observations and modeling of the early acceleration phase of erupting filaments involved in coronal mass ejections
- Formation of a Double-decker Magnetic Flux Rope in the Sigmoidal Solar Active Region 11520
- Sympathetic Magnetic Breakout Coronal Mass Ejections from Pseudostreamers
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