Magnetic topology of coronal mass ejections based on ISEE-3 observations of bidirectional electron fluxes at 1 AU

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The solar wind electron heat flux is carried primarily by superthermal halo'' electrons with energies at 1 AU of {approximately}80 eV and greater. These halo electrons typically are beamed antisunward along the IMF, indicating effective magnetic connection to the Sun only in one direction. However, ISEE-3 electron observations at 1 AU show that counterstreaming halo beams, suggesting closed magnetic structures, prevail within CMEs. These structures might be magnetic tongues,'' tied to the Sun at both ends, magnetically detached plasmoids, or perhaps complex flux rope structures. We present the results of analysis of ISEE-3 electron observations within 39 CMEs. Parameters analyzed ... continued below

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Pages: (7 p)

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Phillips, J.L.; Gosling, J.T.; McComas, D.J.; Bame, S.J. & Feldman, W.C. January 1, 1991.

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The solar wind electron heat flux is carried primarily by superthermal halo'' electrons with energies at 1 AU of {approximately}80 eV and greater. These halo electrons typically are beamed antisunward along the IMF, indicating effective magnetic connection to the Sun only in one direction. However, ISEE-3 electron observations at 1 AU show that counterstreaming halo beams, suggesting closed magnetic structures, prevail within CMEs. These structures might be magnetic tongues,'' tied to the Sun at both ends, magnetically detached plasmoids, or perhaps complex flux rope structures. We present the results of analysis of ISEE-3 electron observations within 39 CMEs. Parameters analyzed include: the asymmetry between the counterstreaming beams, control by the IMF orientation, and the variation of the electron distributions as a particular CME convects past the spacecraft. We find that some CMEs contain nearly symmetric electron beams, while others are strongly asymmetric, and that beam propagating most nearly antisunward is generally dominant. The more nearly radial the IMF the greater is the symmetry between outward and inward beams. Trends observed as CMEs propagate past the spacecraft probably result primarily from the compression of the leading edge. We present examples of a previously unreported strahl-on-strahl'' distribution, suggesting continued magnetic connection to the corona, in which a narrow antisunward beam is superimposed on a broader beam. Preliminary results show that such spectra are present in a substantial fraction of the observed CMEs. Taken as a whole, our results appear to favor a tongue or flux rope scenario rather than a detached plasmoid.

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Pages: (7 p)

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OSTI; NTIS; GPO Dep.

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  • Solar connection with transient interplanetary processes (SOLTIP), Castle Liblice (Czechoslovakia), 30 Sep - 5 Oct 1991

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  • Other: DE92000250
  • Report No.: LA-UR-91-2945
  • Report No.: CONF-9109254--2
  • Grant Number: W-7405-ENG-36
  • Office of Scientific & Technical Information Report Number: 5156076
  • Archival Resource Key: ark:/67531/metadc1052576

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  • January 1, 1991

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  • Jan. 22, 2018, 7:23 a.m.

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  • Feb. 1, 2018, 7:04 p.m.

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Phillips, J.L.; Gosling, J.T.; McComas, D.J.; Bame, S.J. & Feldman, W.C. Magnetic topology of coronal mass ejections based on ISEE-3 observations of bidirectional electron fluxes at 1 AU, article, January 1, 1991; New Mexico. (digital.library.unt.edu/ark:/67531/metadc1052576/: accessed December 16, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.