Energy release in the solar corona from spatially resolved magnetic braids

J. W. Cirtain (), L. Golub, A. R. Winebarger, B. De Pontieu, K. Kobayashi, R. L. Moore, R. W. Walsh, K. E. Korreck, M. Weber, P. McCauley, A. Title, S. Kuzin and C. E. DeForest
Additional contact information
J. W. Cirtain: Marshall Space Flight Center, NASA, Mail Code ZP13, MSFC, Alabama 36812, USA
L. Golub: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street
A. R. Winebarger: Marshall Space Flight Center, NASA, Mail Code ZP13, MSFC, Alabama 36812, USA
B. De Pontieu: Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street
K. Kobayashi: Center for Space and Aeronautic Research, University of Alabama-Huntsville, 320 Sparkman Avenue, Huntsville, Alabama 35812, USA
R. L. Moore: Marshall Space Flight Center, NASA, Mail Code ZP13, MSFC, Alabama 36812, USA
R. W. Walsh: University of Central Lancashire, Preston, Lancashire PR1 2HE, UK
K. E. Korreck: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street
M. Weber: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street
P. McCauley: Harvard-Smithsonian Center for Astrophysics, 60 Garden Street
A. Title: Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street
S. Kuzin: Lebedev Physical Institute, 53 Leninski Prospekt, 119991 Moscow, Russia
C. E. DeForest: Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA

Nature, 2013, vol. 493, issue 7433, 501-503

Abstract: Solar observations at a resolution of 0.2 arc seconds show the reconnection and relaxation of magnetic braids in a coronal active region, leading to the dissipation of sufficient energy to heat the structures to about 4,000,000 K.

Date: 2013
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DOI: 10.1038/nature11772

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