Formation of neutral current sheet and loop coronal transients |
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| Institution: | 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: | An eruption of opposite magnetic flux into a bipolar background field is likely to lead to the formation of a natural current sheet between the new emerging field and the background. A numerical study is made on this process, based on the ideal MMD equations, taking into account the interaction between the magnetic field and the coronal plasma. The result shows that a subsonic eruption will give rise to a four region structure; 1) a cool and dense prominence made of the erupting material in the innermost region; 2) a cool and tenuous region further out; 3) a hot and dense loop formed by the concentration of both the erupting material and the coronal material in the neutral current sheet; and 4) a forerunner region outside the loop with density slightly above the background, due to fast magneto-acoustic waves. This structure agrees with the observed features of typical loop coronal transients. Therefore the eruption of opposite magnetic flux into a bipolar background is probably an important mechanism for triggering off such transients. |
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