Connecting Ephemeral Chromospheric Brightenings to Coronal Loops
Abstract
Sequential chromospheric brightenings (SCBs) flanking solar flares represent chromospheric foot-points of magnetic field lines that extend into the corona. During the eruption of a solar flare related CME, these field lines are considered to be energized in sequence by magnetic re-connection, as coronal fields separate from the solar surface. Using automated procedures to extract physical measurements of chromospheric flares and SCBs, we superpose these features onto coronal EUV images and trace the spatio-temporal relationship between coronal loops and SCBs. We postulate a physical connection for SCBs and their coronal counterparts and estimate an energy budget.
- Publication:
-
AAS/Solar Physics Division Abstracts #42
- Pub Date:
- May 2011
- Bibcode:
- 2011SPD....42.1732K