Connecting Ephemeral Chromospheric Brightenings to Coronal Loops

Details Connecting Ephemeral Chromospheric Brightenings to Coronal Loops Connecting Ephemeral Chromospheric Brightenings to Coronal Loops

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1732k&link_type=abstract

American Astronomical Society, SPD meeting #42, #17.32; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

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.

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