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Power-Law Statistics of Driven Reconnection in the Magnetically Closed CoronaNumerous observations have revealed that power-law distributions are ubiquitous in energetic solar processes. Hard X-rays, soft X-rays, extreme ultraviolet radiation, and radio waves all display power-law frequency distributions. Since magnetic reconnection is the driving mechanism for many energetic solar phenomena, it is likely that reconnection events themselves display such power-law distributions. In this work, we perform numerical simulations of the solar corona driven by simple convective motions at the photospheric level. Using temperature changes, current distributions, and Poynting fluxes as proxies for heating, we demonstrate that energetic events occurring in our simulation display power-law frequency distributions, with slopes in good agreement with observations. We suggest that the braiding-associated reconnection in the corona can be understood in terms of a self-organized criticality model driven by convective rotational motions similar to those observed at the photosphere.
Document ID
Document Type
Reprint (Version printed in journal)
Knizhnik, K. J. (National Academy of Sciences - National Research Council Washington, DC, United States)
Uritskiy, V. M. (Catholic Univ. of America Washington, DC, United States)
Klimchuk, J. A. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
DeVore, C. R. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
May 25, 2018
Publication Date
January 24, 2018
Publication Information
Publication: The Astrophysical Journal
Volume: 853
Issue: 1
Subject Category
Solar Physics
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Funding Number(s)
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