Abstract
A technique for investigating the temporal relationship between Ha filament eruptions and soft X-ray flux is presented. The method is fast, simple, based on statistical measures, and requires no a priori knowledge regarding the location of the filaments on the solar disk. The method is used to study the filament eruption associated with a coronal mass ejection and the M-class flare that originated from NOAA Active Region 9163 on 2000 September 12. The technique provides a quantitative determination of the temporal relationship between changes in the Ha filament and soft X-ray flux. We conclude that the filament eruption begins 2 hr prior to the first detectable enhancement in soft X-ray flux.
Original language | English (US) |
---|---|
Pages (from-to) | L133-L136 |
Journal | Astrophysical Journal |
Volume | 610 |
Issue number | 2 II |
DOIs | |
State | Published - Aug 1 2004 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Methods: statistical
- Stars: flare
- Sun: chromosphere
- Sun: coronal mass ejections (CMEs)
- Sun: filaments
- Techniques: image processing