Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp43c..02p&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SP43C-02
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy
Scientific paper
A leading candidate for the heating of active region (AR) coronal loops is the nanoflare model. This model treats coronal loops as collections of impulsively heated sub-resolution strands and explains several key observational aspects of warm (1-2 MK) coronal loops. However, the basic requirement of this model is that the strands initially reach very high temperatures of several MK before they cool down to canonical coronal temperatures. Therefore, the detection of hot plasmas in AR loops represents a stringest test of the nanoflare model. Previous work has shown that the best way to observe the postulated hot plasmas is by the means of spectroscopic observations in hot lines (T > 3 MK). The emission is predicted to be quite faint, but the EIS spectrometer onboard Hinode has sufficient sensitivity to allow us to perform such a test for the first time. We will present an analysis of the emission characteristics of quiescent coronal loops in a number of hot lines spanning approximately 3-12 MK (Ni XVII, Ca XV, Fe XVII, Ca XVII, Fe XXIII). We will show that hot plasmas are ubiquitous over entire active regions, and we will compare the measured intensities of both hot and warm lines with predictions of nanoflare models.
Klimchuk James A.
Patsourakos Spiros
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