Propagation of the 12 May 1997 interplanetary coronal mass ejection in evolving solar wind structures

2005 ◽  
Vol 110 (A2) ◽  
Author(s):  
D. Odstrcil
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Interplanetary Coronal Mass Ejection ◽  
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.

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.

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.

Flux Rope Model of the 2003 October 28–30 Coronal Mass Ejection and Interplanetary Coronal Mass Ejection

2006 ◽  
Vol 642 (1) ◽  
pp. 541-553 ◽  
Author(s):  
J. Krall ◽  
V. B. Yurchyshyn ◽  
S. Slinker ◽  
R. M. Skoug ◽  
J. Chen
Keyword(s):  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Interplanetary Coronal Mass Ejection ◽  
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

MHD simulations of magnetospheric response to a strong solar wind density pulse

2021 ◽  
Author(s):  
Andrey Samsonov ◽  
Jennifer A. Carter ◽  
Graziella Branduardi-Raymont ◽  
Steven Sembay
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Density ◽  
Ionospheric Currents ◽  
X Ray ◽  
Interplanetary Coronal Mass Ejection ◽  
Explorer Mission ◽  
The One ◽  
Mass Ejection ◽  
Present Simulation

&lt;p&gt;On 16-17 June 2012, an interplanetary coronal mass ejection with an extremely high solar wind density (~100 cm&lt;sup&gt;-3&lt;/sup&gt;) and mostly strong northward (or eastward) interplanetary magnetic field (IMF) interacted with the Earth&amp;#8217;s magnetosphere. We have simulated this event using global MHD models. We study the magnetospheric response to two solar wind discontinuities. The first is characterized by a fast drop of the solar wind dynamic pressure resulting in rapid magnetospheric expansion. The second is a northward IMF turning which causes reconfiguration of the magnetospheric-ionospheric currents. We discuss variations of the magnetopause position and locations of the magnetopause reconnection in response to the solar wind variations. In the second part of our presentation, we present simulation results for the forthcoming SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission. SMILE is scheduled for launch in 2024. We produce two-dimensional images that derive from the MHD results of the expected X-ray emission as observed by the SMILE Soft X-ray Imager (SXI).&amp;#160;We discuss how SMILE observations may help to study events like the one presented in this work.&lt;/p&gt;

A bubblelike coronal mass ejection flux rope in the solar wind

1990 ◽  
pp. 365-371 ◽  
Author(s):  
N. U. Crooker ◽  
J. T. Gosling ◽  
E. J. Smith ◽  
C. T. Russell
Keyword(s):  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Flux Rope ◽  
Mass Ejection

scholarly journals Planar magnetic structures in coronal mass ejection-driven sheath regions

2016 ◽  
Vol 34 (2) ◽  
pp. 313-322 ◽  
Author(s):  
Erika Palmerio ◽  
Emilia K. J. Kilpua ◽  
Neel P. Savani
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Leading Edge ◽  
Formation Mechanisms ◽  
Single Plane ◽  
Magnetic Structures ◽  
Automated Method ◽  
Mass Ejection ◽  
The Magnetic Field

Abstract. Planar magnetic structures (PMSs) are periods in the solar wind during which interplanetary magnetic field vectors are nearly parallel to a single plane. One of the specific regions where PMSs have been reported are coronal mass ejection (CME)-driven sheaths. We use here an automated method to identify PMSs in 95 CME sheath regions observed in situ by the Wind and ACE spacecraft between 1997 and 2015. The occurrence and location of the PMSs are related to various shock, sheath, and CME properties. We find that PMSs are ubiquitous in CME sheaths; 85 % of the studied sheath regions had PMSs with the mean duration of 6 h. In about one-third of the cases the magnetic field vectors followed a single PMS plane that covered a significant part (at least 67 %) of the sheath region. Our analysis gives strong support for two suggested PMS formation mechanisms: the amplification and alignment of solar wind discontinuities near the CME-driven shock and the draping of the magnetic field lines around the CME ejecta. For example, we found that the shock and PMS plane normals generally coincided for the events where the PMSs occurred near the shock (68 % of the PMS plane normals near the shock were separated by less than 20° from the shock normal), while deviations were clearly larger when PMSs occurred close to the ejecta leading edge. In addition, PMSs near the shock were generally associated with lower upstream plasma beta than the cases where PMSs occurred near the leading edge of the CME. We also demonstrate that the planar parts of the sheath contain a higher amount of strong southward magnetic field than the non-planar parts, suggesting that planar sheaths are more likely to drive magnetospheric activity.

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