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Titolo:
Drive mechanisms of erupting solar magnetic flux ropes
Autore:
Krall, J; Chen, J; Santoro, R;
Indirizzi:
USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA USN Washington DCUSA 20375 ab, Div Plasma Phys, Washington, DC 20375 USA USN, Res Lab, Natl Res Council, Washington, DC 20375 USA USN Washington DC USA 20375 b, Natl Res Council, Washington, DC 20375 USA
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 539, anno: 2000,
parte:, 1
pagine: 964 - 982
SICI:
0004-637X(20000820)539:2<964:DMOESM>2.0.ZU;2-Y
Fonte:
ISI
Lingua:
ENG
Soggetto:
CORONAL MASS EJECTIONS; NUMERICAL-SIMULATION; DYNAMICAL EVOLUTION; PROMINENCE MATERIAL; GEOMAGNETIC STORMS; FIELD MEASUREMENTS; CURRENT LOOPS; JANUARY 1997; CLOUDS; WIND;
Keywords:
Sun : activity; Sun : magnetic fields; Sun : prominences;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
99
Recensione:
Indirizzi per estratti:
Indirizzo: Krall, J USN, Res Lab, Div Plasma Phys, Washington, DC 20375 USA USN Washington DC USA 20375 lasma Phys, Washington, DC 20375 USA
Citazione:
J. Krall et al., "Drive mechanisms of erupting solar magnetic flux ropes", ASTROPHYS J, 539(2), 2000, pp. 964-982

Abstract

The dynamics of magnetic flux ropes near the Sun and in interplanetary space are studied using a magnetohydrodynamic model of erupting magnetic flux ropes. In this model, the magnetic structure of a coronal mass ejection (CME) corresponds to a flux rope with footpoints that remain anchored below the photosphere. The model flux rope eruption can be driven by a rapid increase in poloidal flux (flux injection), a quasi-static increase in poloidal flux (photospheric footpoint twisting), a rapid release of stored magnetic energy (magnetic energy release), or a rapid increase in the amount of hot plasma within the flux rope (hot plasma injection). Model results are compared with Large-Angle Spectrometric Coronagraph data (from the CME of 1997 April 13) and with interplanetary magnetic cloud data over the range 0.4-5 AU. Of these mechanisms, only flux injection and magnetic energy release reproduce key features of the data both near the Sun and in the interplanetary medium and only Bur injection obtains a detailed match to the near-Sun dynamics.

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Documento generato il 26/09/20 alle ore 00:20:07