The Role of Isolated EUV Brightenings in Heating the Corona

Details The Role of Isolated EUV Brightenings in Heating the Corona The Role of Isolated EUV Brightenings in Heating the Corona

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp43c..04b&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP43C-04

Physics

7509 Corona, 7524 Magnetic Fields, 7529 Photosphere, 7546 Transition Region, 7549 Ultraviolet Emissions

Scientific paper

Nanoflare reconnection events have been proposed as a mechanism for heating the solar corona. Parker's original suggestion was that frequent reconnection events occur in coronal loops due to the twisting and braiding of the magnetic field. Many observational studies, however, have focused on the radiating properties of isolated brightening events, but their cause, role, and relevance for coronal heating has not yet been established. Using Hinode Solar Optical Telescope (SOT) magnetograms and high cadence EUV Imaging Spectrometer (EIS) slot rasters we study the relationship between transition region and coronal emission and the evolution of the magnetic field. We find that hot, relatively steadily emitting coronal loops are generally rooted in magnetic field regions that are locally unipolar yet highly dynamic, whereas detailed analysis shows that ubiquitous EUV brightenings are found in regions of magnetic flux cancellation in the photosphere. This suggests that the heating in transient events may be fundamentally different than the heating in coronal loops and that they play no direct role in the heating of the quiescent corona.

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