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.

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

scholarly journals Integration of RAM-SCB into the Space Weather Modeling Framework

2018 ◽  
Vol 177 ◽  
pp. 160-168 ◽  
Author(s):  
Daniel T. Welling ◽  
Gabor Toth ◽  
Vania K. Jordanova ◽  
Yiqun Yu
Keyword(s):  
Space Weather ◽  
Modeling Framework ◽  
Weather Modeling

Focused transport of energetic particles along magnetic field lines draped around a coronal mass ejection

1992 ◽  
Vol 97 (A2) ◽  
pp. 1597 ◽  
Author(s):  
L. C. Tan ◽  
G. M. Mason ◽  
M. A. Lee ◽  
B. Klecker ◽  
F. M. Ipavich
Keyword(s):  
Magnetic Field ◽  
Coronal Mass Ejection ◽  
Energetic Particles ◽  
Field Lines ◽  
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 Halloween Storm Simulations with the Space Weather Modeling Framework

2006 ◽  
Author(s):  
Tamas Gombosi ◽  
Gabor Toth ◽  
Igor Sokolov ◽  
Ward Manchester ◽  
Aaron Ridley ◽  
...  
Keyword(s):  
Space Weather ◽  
Modeling Framework ◽  
Weather Modeling

scholarly journals Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby

2021 ◽  
Author(s):  
Martin Volwerk ◽  
Beatriz Sánchez-Cano ◽  
Daniel Heyner ◽  
Sae Aizawa ◽  
Nicolas André ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Interplanetary Magnetic Field ◽  
Bow Shock ◽  
Gravity Assist ◽  
Highly Active ◽  
Field Lines ◽  
Mass Ejection ◽  
The Magnetic Field

Abstract. Out of the two Venus flybys that BepiColombo uses as a gravity assist manoeuvre to finally arrive at Mercury, the first took place on 15 October 2020. After passing the bow shock, the spacecraft travelled along the induced magnetotail, crossing it mainly in the YVSO-direction. In this paper, the BepiColombo Mercury Planetary Orbiter Magnetometer (MPO-MAG) data are discussed, with support from three other plasma instruments: the Planetary Ion Camera (PICAM), the Mercury Electron Analyser (MEA) and the radiation monitor (BERM). Behind the bow shock crossing, the magnetic field showed a draping pattern consistent with field lines connected to the interplanetary magnetic field wrapping around the planet. This flyby showed a highly active magnetotail, with, e.g., strong flapping motions at a period of ~7 min. This activity was driven by solar wind conditions. Just before this flyby, Venus's induced magnetosphere was impacted by a stealth coronal mass ejection, of which the trailing side was still interacting with it during the flyby. This flyby is a unique opportunity to study the full length and structure of the induced magnetotail of Venus, indicating that the tail was most likely still present at about 48 Venus radii.

scholarly journals The Space Weather Modeling Framework Goes Open Access

Eos ◽  
2021 ◽  
Vol 102 ◽  
Author(s):  
Tuija Pulkkinen ◽  
Tamas Gombosi ◽  
Aaron Ridley ◽  
Gabor Toth ◽  
Shasha Zou
Keyword(s):  
Open Access ◽  
Space Weather ◽  
Computational Models ◽  
Power Grid ◽  
Magnetic Storms ◽  
Modeling Framework ◽  
Weather Modeling

A versatile suite of computational models, already used to forecast magnetic storms and potential power grid and telecommunications disruptions, is preparing to welcome a larger group of users.

Formation of solar coronal loops through magnetic reconnection in an emerging active region

2021 ◽  
Author(s):  
Zhenyong Hou ◽  
Hui Tian ◽  
Hechao Chen ◽  
Xiaoshuai Zhu ◽  
Jiansen He ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheet ◽  
Emission Measure ◽  
Three Dimensional ◽  
Transverse Field ◽  
Power Spectral Analysis ◽  
Active Regions ◽  
Building Blocks ◽  
Coronal Loops ◽  
Field Lines

<p>Coronal loops are building blocks of solar active regions (ARs). However, their formation is not well understood. Here we present direct observational evidence for the formation of coronal loops through magnetic reconnection as new magnetic fluxes emerge to the solar atmosphere. Observations in the EUV passbands of SDO/AIA clearly show the newly formed loops following magnetic reconnection within a vertical current sheet. Formation of the loops is also seen in the Hα images taken by NVST. The SDO/HMI observations show that a positive-polarity flux concentration moves toward a negative-polarity one with a speed of ~0.5 km s<sup>-1</sup> before the apparent formation of coronal loops. During the formation of coronal loops, we found signatures of flux cancellation and subsequent enhancement of the transverse field between the two polarities. We have reconstructed the three-dimensional magnetic field structure through a magnetohydrostatic model, which shows field lines consistent with the loops in AIA images. Numerous bright blobs with a width of ~1.5 Mm appear intermittently in the current sheet and move upward with apparent velocities of ~80 km s<sup>-1</sup>. We have also identified plasma blobs moving to the footpoints of the newly formed large loops, with apparent velocities ranging from 30 to 50 km s<sup>-1</sup>. A differential emission measure analysis shows that the temperature, emission measure and density of the bright blobs are 2.5-3.5 MK, 1.1-2.3×10<sup>28</sup> cm<sup>-5</sup> and 8.9-12.9×10<sup>9</sup> cm<sup>-3</sup>, respectively. Power spectral analysis of these blobs indicates that the magnetic reconnection is inconsistent with the turbulent reconnection scenario.</p>

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