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Observational Signatures of Impulsively Heated Coronal Loops: Power-Law Distribution of Energies
Taroyan, Y.; Erdélyi, R.; Bradshaw, S. J.
AA(Institute of Mathematics and Physics, Aberystwyth University, Aberystwyth, UK), AB(SP²RC, Department of Applied Mathematics, University of Sheffield, Sheffield, UK), AC(Department of Physics and Astronomy, Rice University, Houston, USA; Solar Physics Lab., NASA Goddard Space Flight Center, Greenbelt, USA)
Solar Physics, Volume 269, Issue 2, pp.295-307 (SoPh Homepage)
Publication Date:
Heating, coronal, Flares, microflares and nanoflares, Spectral line, intensity and diagnostics
Abstract Copyright:
(c) 2011: Springer Science+Business Media B.V.
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It has been established that small scale heating events, known as nanoflares, are important for solar coronal heating if the power-law distribution of their energies has a slope alpha steeper than -2 ( alpha<-2). Forward modeling of impulsively heated coronal loops with a set of prescribed power-law indices alpha is performed. The power-law distribution is incorporated into the governing equations of motion through an impulsive heating term. The results are converted into synthetic Hinode/EIS observations in the 40" imaging mode, using a selection of spectral lines formed at various temperatures. It is shown that the intensities of the emission lines and their standard deviations are sensitive to changes in alpha. A method based on a combination of observations and forward modeling is proposed for determining whether the heating in a particular case is due to small or large scale events. The method is extended and applied to a loop structure that consists of multiple strands.
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