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Titolo:
Evolution of global-scale coronal magnetic field due to magnetic reconnection: The formation of the observed blob motion in the coronal streamer belt
Autore:
Wu, ST; Wang, AH; Plunkett, SP; Michels, DJ;
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, Univ Space Res Assoc, Washington, DC 20375 USA USN Washington DC USA 20375 niv Space Res Assoc, Washington, DC 20375 USA
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 545, anno: 2000,
parte:, 1
pagine: 1101 - 1115
SICI:
0004-637X(200012)545:2<1101:EOGCMF>2.0.ZU;2-B
Fonte:
ISI
Lingua:
ENG
Soggetto:
EULERIAN FICE SCHEME; MHD FLOWS; MODEL;
Keywords:
MHD; Sun : corona; Sun : magnetic fields;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
28
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., "Evolution of global-scale coronal magnetic field due to magnetic reconnection: The formation of the observed blob motion in the coronal streamer belt", ASTROPHYS J, 545(2), 2000, pp. 1101-1115

Abstract

Recent SOHO/LASCO/EIT observations showed that the global corona at the minimum phase of cycle 22 is an organized, simple, and persistent dipolar configuration streamer belt (Michels). But the low-lying, closed-loop, multipolar magnetic structure of the inner corona at low- to mid-latitudes revealed in EIT and LASCO images is not static. It stretches continuously outward,feeding plasma into higher coronal structures and eventually into the solar wind, including plasma blobs (Sheeley et al.; Wang et al.). To understandthe physics of this slow dynamic evolution process, we use a two-dimensional, planar, resistive MHD model and observed pre-event characteristics for the model input to simulate the formation and propagation of these observedplasma blobs. It seems that reconnection processes among the low-lying multipolar coronal loops and their overlying streamers cause the slow time evolution. The motion of plasma blobs frequently observed by LASCO C2/C3 is indeed reproduced by this model through reconnection in the multipolar loops. Results presented in this paper are the global field evolution, mass, momentum, and energy transport from the inner corona to the outer corona and upinto the streamer belt region where slow solar wind forms. We conclude that these plasma blobs may be the origin of the lumps in the solar wind observed in interplanetary space.

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Documento generato il 29/10/20 alle ore 23:25:46