scholarly journals Three-Dimensional Simulations of Solar Wind Preconditioning and the 23 July 2012 Interplanetary Coronal Mass Ejection

Solar Physics ◽  
2020 ◽  
Vol 295 (9) ◽  
Author(s):  
Ravindra T. Desai ◽  
Han Zhang ◽  
Emma E. Davies ◽  
Julia E. Stawarz ◽  
Joan Mico-Gomez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Large Scale ◽  
Weather Forecasting ◽  
Time Window ◽  
Initial Conditions ◽  
Interplanetary Space ◽  
Three Dimensional ◽  
Interplanetary Coronal Mass Ejection ◽  
Mass Ejection

Abstract Predicting the large-scale eruptions from the solar corona and their propagation through interplanetary space remains an outstanding challenge in solar- and helio-physics research. In this article, we describe three-dimensional magnetohydrodynamic simulations of the inner heliosphere leading up to and including the extreme interplanetary coronal mass ejection (ICME) of 23 July 2012, developed using the code PLUTO. The simulations are driven using the output of coronal models for Carrington rotations 2125 and 2126 and, given the uncertainties in the initial conditions, are able to reproduce an event of comparable magnitude to the 23 July ICME, with similar velocity and density profiles at 1 au. The launch time of this event is then varied with regards to an initial 19 July ICME and the effects of solar wind preconditioning are found to be significant for an event of this magnitude and to decrease over a time-window consistent with the ballistic refilling of the depleted heliospheric sector. These results indicate that the 23 July ICME was mostly unaffected by events prior, but would have traveled even faster had it erupted closer in time to the 19 July event where it would have experienced even lower drag forces. We discuss this systematic study of solar wind preconditioning in the context of space weather forecasting.

scholarly journals Three-dimensional MHD simulation of the 2008 December 12 coronal mass ejection: from the Sun to Interplanetary space

2019 ◽  
Vol 9 ◽  
pp. A33
Author(s):  
Man Zhang ◽  
Xue Shang Feng ◽  
Li Ping Yang
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Coronal Mass Ejection ◽  
Interplanetary Space ◽  
Three Dimensional ◽  
Finite Volume Scheme ◽  
The Sun ◽  
Dynamical Interaction ◽  
Spherical Coordinate ◽  
Mass Ejection

A three-dimensional time-dependent, numerical magnetohydrodynamic simulation is performed to investigate the propagation of a coronal mass ejection that occurred on 12 December 2008. The background solar wind is obtained by using a splitting finite-volume scheme based on a six-component grid system in spherical coordinate, with Parker’s one-dimensional solar wind solution and measured photospheric magnetic fields as the initial values. A spherical plasmoid is superposed on the realistic ambient solar wind to study the 12 December 2008 coronal mass ejection event. The plasmoid is assumed to have a spheromak magnetic structure with a high-density, high-velocity, and high-pressure near the Sun. The dynamical interaction between the coronal mass ejection and the background solar wind flow is then investigated. We compared the model results with observations, and the model provide a relatively satisfactory comparison with the Wind spacecraft observations at 1 AU. We also investigated the numerical results assuming different parameters of the CME, we find that initial magnetic fields in the CME have a larger influence on the solar wind parameters at the Earth.

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

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

High-latitude ionospheric response to co-rotating interaction region- and coronal mass ejection-driven geomagnetic storms revealed by GPS tomography and ionosondes

2010 ◽  
Vol 466 (2123) ◽  
pp. 3391-3408 ◽  
Author(s):  
D. Pokhotelov ◽  
P. T. Jayachandran ◽  
C. N. Mitchell ◽  
M. H. Denton
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Plasma Density ◽  
Large Scale ◽  
Geomagnetic Storms ◽  
Interaction Region ◽  
Electron Content ◽  
Polar Cap ◽  
Total Electron ◽  
Mass Ejection

Positive ionospheric anomalies induced in the polar cap region by co-rotating interaction region (CIR)- and coronal mass ejection (CME)-driven geomagnetic storms are analysed using four-dimensional tomographic reconstructions of the ionospheric plasma density based on measurements of the total electron content along ray paths of GPS signals. The results of GPS tomography are compared with ground-based observations of F region plasma density by digital ionosondes located in the Canadian Arctic. It is demonstrated that CIR- and CME-driven storms can produce large-scale polar cap anomalies of similar morphology in the form of the tongue of ionization (TOI) that appears on the poleward edge of the mid-latitude dayside storm-enhanced densities in positive ionospheric storms. The CIR-driven event of 14–16 October 2002 was able to produce ionospheric anomalies (TOI) comparable to those produced by the CME-driven storms of greater Dst magnitude. From the comparison of tomographic reconstructions and ionosonde data with solar wind measurements, it appears that the formation of large-scale polar cap anomalies is controlled by the orientation of the interplanetary magnetic field (IMF) with the TOI forming during the periods of extended southward IMF under conditions of high solar wind velocity.

THE SOURCE REGIONS OF CORONAL MASS EJECTIONS

2013 ◽  
Vol 23 ◽  
pp. 459-466
Author(s):  
GUIPING ZHOU
Keyword(s):  
Magnetic Flux ◽  
Coronal Mass Ejection ◽  
Coronal Mass Ejections ◽  
Large Scale ◽  
Interplanetary Space ◽  
Activity Analysis ◽  
Angular Width ◽  
Source Regions ◽  
Paper Review ◽  
Mass Ejection

Coronal Mass Ejection is an entire process leading to the ejection of mass and magnetic flux into interplanetary space. Its source is studied by analyzing the associated surface activity. Analysis results show that CMEs have large-scale magnetic source structures, which provide their energy, initiation, and final angular width. This paper review the studies of CME source regions with laying emphasis on their large-scale source structures.

Coexistence of a planar magnetic structure and an Alfvén wave in the shock-sheath of an interplanetary coronal mass ejection

2019 ◽  
Vol 490 (2) ◽  
pp. 1638-1643 ◽  
Author(s):  
Zubair I Shaikh ◽  
Anil Raghav ◽  
Geeta Vichare
Keyword(s):  
Coronal Mass Ejection ◽  
Magnetic Structure ◽  
Interplanetary Space ◽  
Minimum Variance ◽  
Alfven Wave ◽  
Sheath Region ◽  
Interplanetary Coronal Mass Ejection ◽  
Analysis Technique ◽  
Mass Ejection ◽  
First Time

ABSTRACT The excess speed of coronal mass ejection over the ambient solar wind in interplanetary space generates a highly compressed, heated and turbulent shock-sheath. Here, for the first time, we present in situ observations of a unique and distinct feature of the shock-sheath, which exhibits the characteristics of a planar magnetic structure (PMS) and an Alfvén wave simultaneously. We have used standard techniques to confirm the presence of the PMS as described in Shaikh et al. We have employed the minimum variance analysis technique to estimate the properties of the PMS. The Walén test is used to confirm the presence of the Alfvén wave. Our study unambiguously proves the coexistence of the Alfvén wave and the PMS in the shock-sheath region. Further studies are essential to investigate the origin of such a peculiar shock-sheath and its effect on our view of solar-terrestrial physics.

scholarly journals An unusual giant spiral arc in the polar cap region during the northward phase of a Coronal Mass Ejection

2007 ◽  
Vol 25 (2) ◽  
pp. 507-517 ◽  
Author(s):  
L. Rosenqvist ◽  
A. Kullen ◽  
S. Buchert
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Spiral Structure ◽  
Wind Pressure ◽  
Polar Cap ◽  
Sheath Region ◽  
Interplanetary Coronal Mass Ejection ◽  
Solar Wind Pressure ◽  
Pressure Changes ◽  
Mass Ejection

Abstract. The shock arrival of an Interplanetary Coronal Mass Ejection (ICME) at ~09:50 UT on 22 November 1997 resulted in the development of an intense (Dst<−100 nT) geomagnetic storm at Earth. In the early, quiet phase of the storm, in the sheath region of the ICME, an unusual large spiral structure (diameter of ~1000 km) was observed at very high latitudes by the Polar UVI instrument. The evolution of this structure started as a polewardly displaced auroral bulge which further developed into the spiral structure spreading across a large part of the polar cap. This study attempts to examine the cause of the chain of events that resulted in the giant auroral spiral. During this period the interplanetary magnetic field (IMF) was dominantly northward (Bz>25 nT) with a strong duskward component (By>15 nT) resulting in a highly twisted tail plasma sheet. Geotail was located at the equatorial dawnside magnetotail flank and observed accelerated plasma flows exceeding the solar wind bulk velocity by almost 60%. These flows are observed on the magnetosheath side of the magnetopause and the acceleration mechanism is proposed to be typical for strongly northward IMF. Identified candidates to the cause of the spiral structure include a By induced twisted magnetotail configuration, the development of magnetopause surface waves due to the enhanced pressure related to the accelerated magnetosheath flows aswell as the formation of additional magnetopause deformations due to external solar wind pressure changes. The uniqeness of the event indicate that most probably a combination of the above effects resulted in a very extreme tail topology. However, the data coverage is insufficient to fully investigate the physical mechanism behind the observations.

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