Magnetic field re-arrangement after prominence eruption

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It has long been known that magnetic reconnection plays a fundamental role in a variety of solar events. Although mainly invoked in flare problems, large-scale loops interconnecting active regions, evolving coronal hole boundaries, the solar magnetic cycle itself, provide different evidence of phenomena which involve magnetic reconnection. A further example might be given by the magnetic field rearrangement which occurs after the eruption of a prominence. Since most often a prominence reforms after its disappearance and may be observed at about the same position it occupied before erupting, the magnetic field has to undergo a temporary disruption to relax back, ... continued below

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Pages: 6

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Kopp, R.A. & Poletto, G. January 1, 1986.

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Description

It has long been known that magnetic reconnection plays a fundamental role in a variety of solar events. Although mainly invoked in flare problems, large-scale loops interconnecting active regions, evolving coronal hole boundaries, the solar magnetic cycle itself, provide different evidence of phenomena which involve magnetic reconnection. A further example might be given by the magnetic field rearrangement which occurs after the eruption of a prominence. Since most often a prominence reforms after its disappearance and may be observed at about the same position it occupied before erupting, the magnetic field has to undergo a temporary disruption to relax back, via reconnection, to a configuration similar to the previous one. The above sequence of events is best observable in the case of two-ribbon (2-R) flares but most probably is associated with all filament eruptions. Even if the explanation of the magnetic field rearrangement after 2-R flares in terms of reconnection is generally accepted, the lack of a three-dimensional model capable of describing the field reconfiguration, has prevented, up to now, a thorough analysis of its topology as traced by H..cap alpha../x-ray loops. The purpose of the present work is to present a numerical technique which enables one to predict and visualize the reconnected configuration, at any time t, and therefore allows one to make a significant comparison of observations and model predictions throughout the whole process. 5 refs., 3 figs.

Physical Description

Pages: 6

Notes

NTIS, PC A02/MF A01; 1.

Source

  • NASA workshop on coronal and prominence plasmas, Berkeley Springs, WV, USA, 8 Apr 1986

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  • Other: DE86012393
  • Report No.: LA-UR-86-1906
  • Report No.: CONF-8604219-1
  • Grant Number: W-7405-ENG-36
  • Office of Scientific & Technical Information Report Number: 5556464
  • Archival Resource Key: ark:/67531/metadc1092525

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Office of Scientific & Technical Information Technical Reports

Reports, articles and other documents harvested from the Office of Scientific and Technical Information.

Office of Scientific and Technical Information (OSTI) is the Department of Energy (DOE) office that collects, preserves, and disseminates DOE-sponsored research and development (R&D) results that are the outcomes of R&D projects or other funded activities at DOE labs and facilities nationwide and grantees at universities and other institutions.

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  • January 1, 1986

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  • Feb. 10, 2018, 10:06 p.m.

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  • June 4, 2018, 3:18 p.m.

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Kopp, R.A. & Poletto, G. Magnetic field re-arrangement after prominence eruption, article, January 1, 1986; New Mexico. (digital.library.unt.edu/ark:/67531/metadc1092525/: accessed December 15, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.