Numerical modeling of the energy storage and release in solar flares |
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| Affiliation: | 1. Institute of Physics, University of Graz, 8010 Graz, Austria;2. Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, Durham, NH 03824, USA;3. Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;4. Department of Astronomy, University of Maryland, College Park, MD 20742, USA;5. Max-Planck-Institut für Sonnensystemforschung, 37077 Göttingen, Germany;6. Department of Physics, University of Helsinki, FI-00014 Helsinki, Finland;7. Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030, USA;8. Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;9. RAL Space, United Kingdom Research and Innovation – Science & Technology Facilities Council, Harwell Campus, Oxfordshire, OX11 0QX, UK;10. Austrian Space Weather Office, GeoSphere Austria, 8020 Graz, Austria;11. Department of Meteorology, University of Reading, Reading RG6 6BB, UK;12. Institute of Atmospheric Physics, 14100 Prague 4, Czech Republic;13. Leibniz-Institut for Astrophysics Potsdam (AIP), 14482 Potsdam, Germany;14. Institute for Space-Earth Environmental Research, Nagoya University, Nagoya 464-8601, Japan;15. Center for Astrophysics and Space Sciences, University of California San Diego, La Jolla, CA 92093, USA;p. Predictive Science Inc., San Diego, CA 92121, USA;q. Radio Astronomy Centre, National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Tamil Nadu 643001, India;r. Arecibo Observatory, University of Central Florida, Arecibo, PR 00612, USA;s. Indian Institute of Astrophysics, Bengaluru 560034, India;t. Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France;u. IRAP, Université Toulouse III — Paul Sabatier, CNRS, CNES, 31028 Toulouse, France;v. Centre for mathematical Plasma Astrophysics (CmPA), KU Leuven, 3001 Leuven, Belgium;w. Solar–Terrestrial Centre of Excellence—SIDC, Royal Observatory of Belgium, 1180 Brussels, Belgium;x. Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, AL 35805, USA;y. CIRES, University of Colorado at Boulder, Boulder, CO 80309, USA;z. Narula Institute of Technology, Kolkata, West Bengal 700109, India;1. US Naval Research Laboratory, 4555 Overlook Ave, SW, Washington, DC 20375, USA;2. Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;3. NorthWest Research Associates, 3380 Mitchell Ln, Boulder, CO 80301, USA;4. High Altitude Observatory, National Center for Atmospheric Research, 3080 Center Green Drive, Boulder, CO 80301, USA;5. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305-4085, USA;6. Space Sciences Laboratory, University of California–Berkeley, 7 Gauss Way, Berkeley, CA 94720, USA;7. Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, 1234 Innovation Drive, Boulder, CO 80303, USA;8. National Solar Observatory, University of Colorado Boulder, 3665 Discovery Drive, Boulder, CO 80303, USA;9. Institute of Solar-Terrestrial Physics of SB RAS, Irkutsk, Russia;10. DKIST Ambassador, USA;11. CSIRO, Space & Astronomy, PO Box 76, Epping, NSW 1710, Australia;12. Astronomy Department, University of Maryland, College Park, MD 20742, USA;13. Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover St. B/252, Palo Alto, CA 94304, USA;14. Air Force Research Laboratory, Space Vehicles Directorate, Kirtland AFB, NM, USA;15. Department of Astrophysical and Planetary Sciences, University of Colorado Boulder, Boulder, CO 80303, USA;p. Predictive Science Inc., San Diego, CA 92121, USA;q. Natural & Applied Sciences, University of Wisconsin–Green Bay, 2420 Nicolet Drive, Green Bay, WI 54311, USA |
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| Abstract: | This paper reports on investigation of the photospheric magnetic fieldline footpoint motion (usually referred to as shear motion) and magnetic flux emerging from below the surface in relation to energy storage in a solar flare. These causality relationships are demonstrated by using numerical magnetohydrodynamic simulations. From these results, one may conclude that the energy stored in solar flares is in the form of currents. The dynamic process through which these currents reach a critical value is discussed as well as how these currents lead to energy release, such as the explosive events of solar flares. |
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