A Time‐dependent Three‐dimensional Magnetohydrodynamic Model of the Coronal Mass Ejection

1998 ◽  
Vol 493 (1) ◽  
pp. 460-473 ◽  
Author(s):  
S. E. Gibson ◽  
B. C. Low
Keyword(s):  
Coronal Mass Ejection ◽  
Three Dimensional ◽  
Time Dependent ◽  
Magnetohydrodynamic Model ◽  
Mass Ejection

scholarly journals Three-dimensional MHD modeling of the solar wind structures associated with 13 December 2006 coronal mass ejection

2009 ◽  
Vol 114 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
R. Kataoka ◽  
T. Ebisuzaki ◽  
K. Kusano ◽  
D. Shiota ◽  
S. Inoue ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Three Dimensional ◽  
Mhd Modeling ◽  
Mass Ejection

THREE-DIMENSIONAL POLARIMETRIC CORONAL MASS EJECTION LOCALIZATION TESTED THROUGH TRIANGULATION

2010 ◽  
Vol 712 (1) ◽  
pp. 453-458 ◽  
Author(s):  
Thomas G. Moran ◽  
Joseph M. Davila ◽  
William T. Thompson
Keyword(s):  
Coronal Mass Ejection ◽  
Three Dimensional ◽  
Mass Ejection

MORPHOLOGICAL EVOLUTION OF A THREE-DIMENSIONAL CORONAL MASS EJECTION CLOUD RECONSTRUCTED FROM THREE VIEWPOINTS

2012 ◽  
Vol 751 (1) ◽  
pp. 18 ◽  
Author(s):  
L. Feng ◽  
B. Inhester ◽  
Y. Wei ◽  
W. Q. Gan ◽  
T. L. Zhang ◽  
...  
Keyword(s):  
Coronal Mass Ejection ◽  
Morphological Evolution ◽  
Three Dimensional ◽  
Mass Ejection

scholarly journals Nanodust dynamics during a coronal mass ejection

2017 ◽  
Vol 35 (5) ◽  
pp. 1033-1049 ◽  
Author(s):  
Andrzej Czechowski ◽  
Jens Kleimann
Keyword(s):  
Magnetic Field ◽  
Coronal Mass Ejection ◽  
Equations Of Motion ◽  
Dust Cloud ◽  
Field Configuration ◽  
Time Dependent ◽  
Computational Domain ◽  
The Sun ◽  
Keplerian Orbits ◽  
Mass Ejection

Abstract. The dynamics of nanometer-sized grains (nanodust) is strongly affected by electromagnetic forces. High-velocity nanodust was proposed as an explanation for the voltage bursts observed by STEREO. A study of nanodust dynamics based on a simple time-stationary model has shown that in the vicinity of the Sun the nanodust is trapped or, outside the trapped region, accelerated to high velocities. We investigate the nanodust dynamics for a time-dependent solar wind and magnetic field configuration in order to find out what happens to nanodust during a coronal mass ejection (CME). The plasma flow and the magnetic field during a CME are obtained by numerical simulations using a 3-D magnetohydrodynamic (MHD) code. The equations of motion for the nanodust particles are solved numerically, assuming that the particles are produced from larger bodies moving in near-circular Keplerian orbits within the circumsolar dust cloud. The charge-to-mass ratios for the nanodust particles are taken to be constant in time. The simulation is restricted to the region within 0.14 AU from the Sun. We find that about 35 % of nanodust particles escape from the computational domain during the CME, reaching very high speeds (up to 1000 km s−1). After the end of the CME the escape continues, but the particle velocities do not exceed 300 km s−1. About 30 % of all particles are trapped in bound non-Keplerian orbits with time-dependent perihelium and aphelium distances. Trapped particles are affected by plasma ion drag, which causes contraction of their orbits.

scholarly journals The August 24, 2002 coronal mass ejection: when a western limb event connects to earth

2008 ◽  
Vol 4 (S257) ◽  
pp. 391-398 ◽  
Author(s):  
Noé Lugaz ◽  
Ilia I. Roussev ◽  
Igor V. Sokolov
Keyword(s):  
Coronal Mass Ejection ◽  
Space Weather ◽  
Three Dimensional ◽  
Active Regions ◽  
Modeling Framework ◽  
Initiation Mechanism ◽  
Weather Modeling ◽  
Field Lines ◽  
Mass Ejection ◽  
Western Limb

AbstractWe discuss how some coronal mass ejections (CMEs) originating from the western limb of the Sun are associated with space weather effects such as solar energetic particles (SEPs), shocks or geo-effective ejecta at Earth. We focus on the August 24, 2002 coronal mass ejection, a fast (~2000 km s−1) eruption originating from W81. Using a three-dimensional magneto-hydrodynamic simulation of this ejection with the Space Weather Modeling Framework (SWMF), we show how a realistic initiation mechanism enables us to study the deflection of the CME in the corona and the heliosphere. Reconnection of the erupting magnetic field with that of neighboring streamers and active regions modify the solar connectivity of the field lines connecting to Earth and can also partly explain the deflection of the eruption during the first tens of minutes. Comparing the results at 1 AU of our simulation with observations by the ACE spacecraft, we find that the simulated shock does not reach Earth, but has a maximum angular span of about 120°, and reaches 35° West of Earth in 58 hours. We find no significant deflection of the CME and its associated shock wave in the heliosphere, and we discuss the consequences for the shock angular span.

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