Deflection of coronal mass ejection in the interplanetary medium

Wang, Yuming; Shen, Chenglong; Wang, S.; Ye, Pinzhong

doi:10.1023/b:sola.0000043576.21942.aa

Cited by 142 publications

(157 citation statements)

References 26 publications

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“…9). This westward bias is consistent with previous results finding that fast western CMEs are more likely to be deflected eastward and intersect the Earth due to interactions with the slower Parker spiral material in front of them (e.g., Zhang et al 2003;Cane & Richardson 2003;Wang et al 2004;Siscoe et al 2007), while slow CMEs are more likely to be deflected westward by the faster Parker spiral material behind them ( Kim et al 2005). The average speed of ICMEs in this study is 520 km s À1 , which is faster than the typical slow solar wind speed and consistent with the westward bias that we find.…”

Section: Icme Parameter Dependence On Source Longitude and Associatedsupporting

confidence: 91%

Analysis of Interplanetary Coronal Mass Ejection Parameters as a Function of Energetics, Source Location, and Magnetic Structure

Reinard

2008

ApJ

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We describe a study of how ICME parameters vary as function of source location, associated flare magnitude, and magnetic structure. The strongest compositional enhancements are found to occur in events originating in central longitudes of the Sun, those with large associated flares, and those that are identified as magnetic clouds. In situ velocity is highest for events associated with large flares. Density has a strong negative correlation with associated flare size, but no strong trend with source longitude or magnetic cloud structure. Temperature is lower than expected for events originating in central longitudes, events associated with large flares, and for magnetic clouds. Total magnetic field is highest for events originating in central longitudes and for magnetic clouds. Combining these results, we suggest that ICMEs may have a basic structure consisting of a core (or cores) of magnetic cloud plasma and compositional signatures that are modulated by CME energetics, surrounded by an envelope with weaker signatures. If this core/envelope scenario is proven to be valid, that suggests that a larger percentage of energetic ICMEs may contain enhanced composition that is not detected by the current single track observations.

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Section: Icme Parameter Dependence On Source Longitude and Associatedsupporting

confidence: 91%

Analysis of Interplanetary Coronal Mass Ejection Parameters as a Function of Energetics, Source Location, and Magnetic Structure

Reinard

2008

ApJ

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“…3 CME and ICME Deflection 3.1 Characteristics and Causes of CME Deflection CME deflection is the departure from a radial trajectory that commonly occurs with significant in-course changes in direction (e.g., Vandas et al 1996;Wang et al 2004;Lugaz et al 2011;Kay et al 2013Kay et al , 2016. Figure 4 shows a clear example of deflection for the 2 November 2008 event where the CME's change in latitude is obvious when comparing the STEREO-B COR1 to COR2 images.…”

Section: Icmes and Magnetic Cloudsmentioning

confidence: 99%

“…These deflections can be attributed to two primary causes: First, magnetic forces produced by the background corona (e.g., MacQueen et al 1986;Kilpua et al 2009;, including the active region of origin . Second, the background solar wind flow pattern can inhibit the latitudinal expansion of the CME in the corona (e.g., ) and the wind also interacts with ICMEs farther out in the heliosphere (e.g., Wang et al 2004). Magnetic forces control the deflection low in the corona, while the importance of kinematic interactions increases at larger heliospheric distances.…”

Section: Icmes and Magnetic Cloudsmentioning

confidence: 99%

“…However, longitudinal deflections are largely controlled by kinematic interactions (e.g., Wang et al 2004) that occur at larger distances in the corona and heliosphere. The main source of longitudinal deflection is caused by interaction of ICMEs with the Parker spiral structured solar wind that occurs when there is sufficient speed difference with the ICME (Wang et al 2004).…”

Section: Icmes and Magnetic Cloudsmentioning

confidence: 99%

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The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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“…Schwenn et al (2005) found the respective rates of false and missing alarms for this correlation to be 15 and 20 percent, which underlines the need for more sophisticated approaches. A first correction is the tendency of the Parker spiral magnetic field to cause a slight westward deflection for fast CMEs, and a stronger eastward deflection for the slower ones (Wang et al, 2004). From a sample of 841 CME observations using the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) mission, St.…”

Section: Trajectory Mappingmentioning

confidence: 99%

4π Models of CMEs and ICMEs (Invited Review)

Kleimann¹

2012

Sol Phys

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Coronal mass ejections (CMEs), which dynamically connect the solar surface to the far reaches of interplanetary space, represent a major manifestation of solar activity. They are not only of principal interest but also play a pivotal role in the context of space weather predictions. The steady improvement of both numerical methods and computational resources during recent years has allowed for the creation of increasingly realistic models of interplanetary CMEs (ICMEs), which can now be compared to high-quality observational data from various space-bound missions. This review discusses existing models of CMEs, characterizing them by scientific aim and scope, CME initiation method, and physical effects included, thereby stressing the importance of fully 3-D ('4π') spatial coverage.

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Deflection of coronal mass ejection in the interplanetary medium

Cited by 142 publications

References 26 publications

Analysis of Interplanetary Coronal Mass Ejection Parameters as a Function of Energetics, Source Location, and Magnetic Structure

Analysis of Interplanetary Coronal Mass Ejection Parameters as a Function of Energetics, Source Location, and Magnetic Structure

The Physical Processes of CME/ICME Evolution

4π Models of CMEs and ICMEs (Invited Review)

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