What can we learn from the geoeffectiveness of the magnetic cloud on 15-17, July 2012?

2021 ◽  
Author(s):  
Gui-Ang Liu ◽  
Ming-Xian Zhao ◽  
Guiming Le ◽  
Tian Mao
Keyword(s):  
Magnetic Cloud

scholarly journals Flux rope axis geometry of magnetic clouds deduced from in situ data

2013 ◽  
Vol 8 (S300) ◽  
pp. 265-268
Author(s):  
Miho Janvier ◽  
Pascal Démoulin ◽  
Sergio Dasso
Keyword(s):  
Interplanetary Medium ◽  
Magnetic Cloud ◽  
Flux Rope ◽  
Magnetic Clouds ◽  
Direct Integration ◽  
Axis Orientation ◽  
In Situ Data ◽  
Geometrical Features ◽  
Wide Range

AbstractMagnetic clouds (MCs) consist of flux ropes that are ejected from the low solar corona during eruptive flares. Following their ejection, they propagate in the interplanetary medium where they can be detected by in situ instruments and heliospheric imagers onboard spacecraft. Although in situ measurements give a wide range of data, these only depict the nature of the MC along the unidirectional trajectory crossing of a spacecraft. As such, direct 3D measurements of MC characteristics are impossible. From a statistical analysis of a wide range of MCs detected at 1 AU by the Wind spacecraft, we propose different methods to deduce the most probable magnetic cloud axis shape. These methods include the comparison of synthetic distributions with observed distributions of the axis orientation, as well as the direct integration of observed probability distribution to deduce the global MC axis shape. The overall shape given by those two methods is then compared with 2D heliospheric images of a propagating MC and we find similar geometrical features.

scholarly journals Main Cause of the Poloidal Plasma Motion Inside a Magnetic Cloud Inferred from Multiple-Spacecraft Observations

Solar Physics ◽  
2017 ◽  
Vol 292 (4) ◽  
Author(s):  
Ake Zhao ◽  
Yuming Wang ◽  
Yutian Chi ◽  
Jiajia Liu ◽  
Chenglong Shen ◽  
...  
Keyword(s):  
Magnetic Cloud ◽  
Plasma Motion ◽  
Multiple Spacecraft

scholarly journals Specific interplanetary conditions for CIR-, Sheath-, and ICME-induced geomagnetic storms obtained by double superposed epoch analysis

2010 ◽  
Vol 28 (12) ◽  
pp. 2177-2186 ◽  
Author(s):  
Yu. I. Yermolaev ◽  
N. S. Nikolaeva ◽  
I. G. Lodkina ◽  
M. Yu. Yermolaev
Keyword(s):  
Large Scale ◽  
Geomagnetic Storms ◽  
Magnetic Cloud ◽  
Magnetic Storms ◽  
Main Phase ◽  
Corotating Interaction Region ◽  
Superposed Epoch Analysis ◽  
Epoch Analysis ◽  
Archive Data ◽  
Scale Types

Abstract. A comparison of specific interplanetary conditions for 798 magnetic storms with Dst <−50 nT during 1976–2000 was made on the basis of the OMNI archive data. We categorized various large-scale types of solar wind as interplanetary drivers of storms: corotating interaction region (CIR), Sheath, interplanetary CME (ICME) including both magnetic cloud (MC) and Ejecta, separately MC and Ejecta, and "Indeterminate" type. The data processing was carried out by the method of double superposed epoch analysis which uses two reference times (onset of storm and minimum of Dst index) and makes a re-scaling of the main phase of the storm in a such way that all storms have equal durations of the main phase in the new time reference frame. This method reproduced some well-known results and allowed us to obtain some new results. Specifically, obtained results demonstrate that (1) in accordance with "output/input" criteria the highest efficiency in generation of magnetic storms is observed for Sheath and the lowest one for MC, and (2) there are significant differences in the properties of MC and Ejecta and in their efficiencies.

scholarly journals Energetic-particle-flux decreases related to magnetic cloud passages as observed by the Helios 1 and 2 spacecraft

2013 ◽  
Vol 556 ◽  
pp. A146 ◽  
Author(s):  
J. J. Blanco ◽  
M. A. Hidalgo ◽  
R. Gómez-Herrero ◽  
J. Rodríguez-Pacheco ◽  
B. Heber ◽  
...  
Keyword(s):  
Energetic Particle ◽  
Particle Flux ◽  
Magnetic Cloud ◽  
Energetic Particle Flux

scholarly journals Understanding the Twist Distribution Inside Magnetic Flux Ropes by Anatomizing an Interplanetary Magnetic Cloud

2018 ◽  
Vol 123 (5) ◽  
pp. 3238-3261 ◽  
Author(s):  
Yuming Wang ◽  
Chenglong Shen ◽  
Rui Liu ◽  
Jiajia Liu ◽  
Jingnan Guo ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Magnetic Cloud ◽  
Magnetic Flux Ropes ◽  
Flux Ropes

scholarly journals The Wind magnetic cloud and events of October 18–20, 1995: Interplanetary properties and as triggers for geomagnetic activity

1997 ◽  
Vol 102 (A7) ◽  
pp. 14049-14063 ◽  
Author(s):  
R. P. Lepping ◽  
L. F. Burlaga ◽  
A. Szabo ◽  
K. W. Ogilvie ◽  
W. H. Mish ◽  
...  
Keyword(s):  
Geomagnetic Activity ◽  
Magnetic Cloud

Observations in the sheath region ahead of a magnetic cloud and in the dayside magnetosheath during magnetic cloud passage

1994 ◽  
Vol 14 (7) ◽  
pp. 105-110 ◽  
Author(s):  
C.J. Farrugia ◽  
R.J. Fitzenreiter ◽  
L.F. Burlaga ◽  
N.V. Erkaev ◽  
V.A. Osherovich ◽  
...  
Keyword(s):  
Magnetic Cloud ◽  
Sheath Region

scholarly journals Numerical study of the reconnection process between magnetic cloud and heliospheric current sheet

2018 ◽  
Vol 619 ◽  
pp. A82
Author(s):  
Man Zhang ◽  
Yu Fen Zhou ◽  
Xue Shang Feng ◽  
Bo Li ◽  
Ming Xiong
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheet ◽  
Dynamic Process ◽  
Large Scale ◽  
Magnetic Cloud ◽  
Numerical Study ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Reconnection Process ◽  
Magnetic Filed

In this paper, we have used a three-dimensional numerical magnetohydrodynamics model to study the reconnection process between magnetic cloud and heliospheric current sheet. Within a steady-state heliospheric model that gives a reasonable large-scale structure of the solar wind near solar minimum, we injected a spherical plasmoid to mimic a magnetic cloud. When the magnetic cloud moves to the heliospheric current sheet, the dynamic process causes the current sheet to become gradually thinner and the magnetic reconnection begin. The numerical simulation can reproduce the basic characteristics of the magnetic reconnection, such as the correlated/anticorrelated signatures in V and B passing a reconnection exhaust. Depending on the initial magnetic helicity of the cloud, magnetic reconnection occurs at points along the boundary of the two systems where antiparallel field lines are forced together. We find the magnetic filed and velocity in the MC have a effect on the reconnection rate, and the magnitude of velocity can also effect the beginning time of reconnection. These results are helpful in understanding and identifying the dynamic process occurring between the magnetic cloud and the heliospheric current sheet.

scholarly journals Investigating the observational signatures of magnetic cloud substructure

2011 ◽  
Vol 116 (A1) ◽  
pp. n/a-n/a ◽  
Author(s):  
K. Steed ◽  
C. J. Owen ◽  
P. Démoulin ◽  
S. Dasso
Keyword(s):  
Magnetic Cloud
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