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Titolo:
Coronal mass ejections (CMEs) initiation: models and observations
Autore:
Wu, ST; Guo, WP; Plunkett, SP; Schmieder, B; Simnett, GM;
Indirizzi:
Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA Univ Alabama Huntsville AL USA 35899 eronom Res, Huntsville, AL 35899 USA Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA Univ Alabama Huntsville AL USA 35899 erosp Engn, Huntsville, AL 35899 USA USN, Res Lab, EO Hulburt Ctr Space Res, Univ Space Res Assoc, Washington, DC 20375 USA USN Washington DC USA 20375 niv Space Res Assoc, Washington, DC 20375 USA Observ Paris, DASOP, F-92195 Meudon, France Observ Paris Meudon France F-92195 Paris, DASOP, F-92195 Meudon, France Univ Birmingham, Sch Phys & Space Res, Space Res Grp, Birmingham B15 2TT, W Midlands, England Univ Birmingham Birmingham W Midlands England B15 2TT W Midlands, England
Titolo Testata:
JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
fascicolo: 16, volume: 62, anno: 2000,
pagine: 1489 - 1498
SICI:
1364-6826(200011)62:16<1489:CME(IM>2.0.ZU;2-Z
Fonte:
ISI
Lingua:
ENG
Soggetto:
MAGNETIC-FIELDS; MAGNETOHYDRODYNAMIC SIMULATION; ERUPTIVE PROMINENCE; DYNAMICAL EVOLUTION; SOLAR CORONA; FLUX ROPE; STREAMER; MHD; FLARES; LASCO;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
35
Recensione:
Indirizzi per estratti:
Indirizzo: Wu, ST Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35899 USA Univ Alabama Huntsville AL USA 35899 Res, Huntsville, AL 35899 USA
Citazione:
S.T. Wu et al., "Coronal mass ejections (CMEs) initiation: models and observations", J ATMOS S-P, 62(16), 2000, pp. 1489-1498

Abstract

We use three observed coronal mass ejection (CME) events and numerical magnetohydrodynamic simulation models to illustrate three distinct CME initiation processes: (1) streamer destabilization due to increase of currents, via increase of axial fields, of the flux-rope, (2) photospheric shear and (3) plasma flow induced CME. The 3 January 1998 event is used to illustrate the streamer destabilization process to initiate a CME because the observed height-time curve indicates that the prominence eruption proceeds the CME initiation. We interpret this CME as being initiated because of destabilization of the streamer due to the upward motion of the flux-rope by the additional Lorentz (J x B) force. On the other hand, the 22 June 1998 event showsthat the CME was launched prior to the prominence eruption. This case is modeled by shear-induced loss-of-equilibrium The last case is entirely different from the previous two. The morphology of the 5 October 1996 event doesnot show any relation with the filament/flux-rope. We modeled this event by introducing a plasma flow. Using the observations and MHD models, we conclude that the first two categories are flux-rope driven, because the energysource, which propels the CME, is stored in the flux-rope, and the third category is driven by an assumed plasma flow with the effects of fast solar wind, because this CME appears at the boundary region of a streamer and coronal hole. (C) 2000 Elsevier Science Ltd. All rights reserved.

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Documento generato il 21/09/20 alle ore 15:54:34