Flare Cooling and Implications for Hinode/EIS

Details Flare Cooling and Implications for Hinode/EIS Flare Cooling and Implications for Hinode/EIS

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..397..184r&link_type=abstract

First Results From Hinode ASP Conference Series, Vol. 397, Proceedings of the conference held 20-24 August, 2007, at Trinity Col

Astronomy and Astrophysics

Astronomy

Scientific paper

The cooling of a post-flare loop system as observed by TRACE and SOHO/CDS, SOHO/EIT, GOES and RHESSI is studied and compared to the predictions of recent solar flare models. The observed C-class flare cools from ≥ 10 MK to ˜ 0.25 MK in approximately 45 mins via conduction and radiation. Using theoretical modelling, conduction was found to dominate during the first 3 min of the decay phase, after which radiation became the dominant loss mechanism (˜ 30 min). We aim to study the flare cooling process using high resolution observations from Hinode/EIS.

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