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Nonlinear Processes in Geophysics An interactive open-access journal of the European Geosciences Union
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Volume 23, issue 4
Nonlin. Processes Geophys., 23, 175–188, 2016
https://doi.org/10.5194/npg-23-175-2016
© Author(s) 2016. This work is distributed under
the Creative Commons Attribution 3.0 License.
Nonlin. Processes Geophys., 23, 175–188, 2016
https://doi.org/10.5194/npg-23-175-2016
© Author(s) 2016. This work is distributed under
the Creative Commons Attribution 3.0 License.

Research article 08 Jul 2016

Research article | 08 Jul 2016

Multi-scale statistical analysis of coronal solar activity

Diana Gamborino et al.

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Subject: Predictability, Data Assimilation | Topic: Ionosphere, Magnetosphere, Planetary Science, Solar Science
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Cited articles

Abramenko, V. I., Yurchyshyn, V. B., Wang, H., Spirok, T. J., and Goode, P. R.: Signature of an avalanche in solar flares as mesaured by photospheric magnetic fields, Astrophys. J., 597, 1135–1144, 2003.
Aschwanden, M. J.: Image processing techiniques and feature recognition in solar physics, Solar Phys., 262, 235–275, https://doi.org/10.1007/s11207-009-9474-y, 2010.
Aschwanden, M. J.: The spatio-temporal evolution of solar flares observed with aia/sdo: fractal diffusion, sub-diffusion, or logistic growth?, Ap. J., 757, 94–115, https://doi.org/10.1088/0004-637X/757/1/94, 2012.
Aschwanden, M. J. and Boerner, P.: Solar corona loop studies with the atmospheric imaging assembly. I. cross-sectional temperature structure, Ap. J., 732, 81, https://doi.org/10.1088/0004-637X/732/2/81, 2011.
Aschwanden, M. J., Boerner, P., Schrijver, C. J., and Malanushenko, A.: Automated Temperature and Emission Measure Analysis of Coronal Loops and Active Regions Observed with the AIA on the SDO, Solar Phys., 283, 5–30, 2013.
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Short summary
We use temperature maps of the solar corona for three regions and use a technique that separates multiple timescales and space scales to show that the small-scale temperature fluctuations appear more frequently prior to the occurrence of a solar flare, in comparison with the same region after the flare and with a quiet region. We find that, during the flare, energy flows from large to small scales and heat transport associated with a heat front is convective along and diffusive across the front.
We use temperature maps of the solar corona for three regions and use a technique that separates...
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