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The Inconvenient Truth About Coronal Dimmings View all abstracts by submitter

Scott McIntosh   Submitted: 2008-11-24 13:46

We investigate the occurrence of a CME-driven coronal dimming using unique high resolution spectral images of the corona from the Hinode spacecraft. Over the course of the dimming event we observe the dynamic increase of non-thermal line broadening in the 195.12? emission line of Fe XII as the corona opens. As the corona begins to close, refill and brighten, we see a reduction of the non-thermal broadening towards the pre-eruption level. We propose that the dynamic evolution of non-thermal broadening is the result of the growth of Alfvén wave amplitudes in the magnetically open rarefied dimming region, compared to the dense closed corona prior to the CME. We suggest, based on this proposition, that, as open magnetic regions, coronal dimmings must act just as coronal holes and be sources of the fast solar wind, but only temporarily. Further, we propose that such a rapid transition in the thermodynamics of the corona to a solar wind state may have an impulsive effect on the CME that initiates the observed dimming. This last point, if correct, poses a significant physical challenge to the sophistication of CME modeling and capturing the essence of the source region thermodynamics necessary to correctly ascertain CME propagation speeds, etc.

Authors: Scott W. McIntosh
Projects: Hinode/EIS

Publication Status: Submitted ApJ - rerouted to ApJL
Last Modified: 2008-11-25 05:50
Go to main E-Print page  Solar Radio Spikes in 2.6-3.8 GHz for 13 December 2006 Event  The Solar Wind at 1 AU During the Declining Phase of Solar Cycle 23: Comparison of 3D Numerical Model Results with Observations  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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