Revisiting Ribbon Fluxes and CME Speeds
Abstract
The dynamics of coronal mass ejections (CMEs) remain poorly understood. A previous study found that the final speeds of CMEs were strongly correlated with the amount of photospheric magnetic flux swept out by flare ribbons. The latter quantity, which we refer to as the ribbon flux, is thought to be directly related to the amount of coronal magnetic flux that reconnects during an eruption. The prior study, however, analyzed flare ribbons associated with a small sample (N=13) of relatively fast CMEs (all > 600 km/s, mean speed > 1300 km/s). With the launch of the Solar Dynamics Observatory (SDO) in 2010, automated co-registration of ribbon images observed in UV by its Atmospheric Imaging Assembly (AIA) with line-of-sight magnetograms observed by its Helioseismic and Magnetic Imager (HMI) enabled compilation of a relatively large database of ribbon fluxes. Here, we characterize relationships between ribbon fluxes and the speeds (and other properties) of manually-associated CMEs in a sample of several dozen events.
- Publication:
-
AAS/Solar Physics Division Abstracts #47
- Pub Date:
- May 2016
- Bibcode:
- 2016SPD....47.0338W