MHD numerical study of the latitudinal deflection of coronal mass ejection

Zhou, Yufen; Feng, Xueshang

doi:10.1002/2013ja018976

Cited by 33 publications

(26 citation statements)

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“…Kay, Opher, and Evans (2013) have developed a method for predicting CME propagation directions that include both magnetic pressure and magnetic tension forces; they find that the tension forces can be strong. It is also possible that the orientation of the CME magnetic field with respect to the neighboring coronal fields will affect the trajectory of the CME, as seen in the simulations of Zhou and Feng (2013).…”

Section: Observations and Methods Of Analysismentioning

confidence: 99%

Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun

et al. 2015

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The trajectories of coronal mass ejection (CME) are often observed to deviate from radial propagation from the source while within the coronagraph field of view (R < 15 -30 R sun ). To better understand nonradial propagation within the corona, we first analyze the trajectories of five CMEs for which both the source and 3D trajectory (latitude, longitude, and velocity) can be well determined from solar imaging observations, primarily using observations from the twin Solar TErrestrial RElations Observatory (STEREO) spacecraft. Next we analyze the cause of any nonradial propagation using a potential field source surface (PFSS) model to determine the direction of the magnetic pressure forces exerted on the CME at various heights in the corona. In two cases, we find that the CME deviation from radial propagation primarily occurs before it reaches the coronagraph field of view (below 1.5 solar radii). Based on the observations and the magnetic pressure forces calculated from the PFSS model, we conclude that for these cases the deviation is the result of strong active-region fields causing an initial asymmetric expansion of the CME that gives rise to the apparent rapid deflection and nonradial propagation from the source. Within the limitations of the PFSS model, the magnetic fields for all five cases appear to guide the CMEs out of the corona through the weak-field region around the heliospheric current sheet even when the current sheet is inclined and warped.

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Section: Observations and Methods Of Analysismentioning

confidence: 99%

Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun

et al. 2015

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“…The CESE method has been successfully used and shown its powerful capability in space weather modeling [Feng et al, 2007[Feng et al, , 2011[Feng et al, , 2012Zhou and Feng, 2013]. The CESE method treats space and time as a unity, which is the key difference between the CESE method and most existing numerical difference schemes.…”

Section: The Cese Methodsmentioning

confidence: 99%

Modeling the interaction between the solar wind and Saturn's magnetosphere by the AMR‐CESE‐MHD method

Wang

Feng

et al. 2014

JGR Space Physics

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In this paper, the space‐time conservation element and solution element (CESE) method in general curvilinear coordinates is successfully applied to the three‐dimensional magnetohydrodynamic (MHD) simulations of the interaction between the solar wind and Saturn's magnetosphere on a six‐component grid system. As a new numerical model modified for the study of the interaction between the solar wind and Saturn's magnetosphere, we obtain the large‐scale configurations of Saturn's magnetosphere under the steady solar wind with due southward interplanetary magnetic field (IMF) conditions. The numerical results clearly indicate that the global structure of Saturn's magnetosphere is strongly affected by the rotation of Saturn as well as by the solar wind. The subsolar standoff distances of the magnetopause and the bow shock in our model are consistent with those predicted by the data‐based empirical models. Our MHD results also show that a plasmoid forms in the magnetotail under the effect of the fast planetary rotation. However, somewhat differently from the previous models, we find that there are two flow vortices generated on the duskside under due southward IMF at Saturn. On the duskside, the clockwise one closer to the planet is excited by the velocity shear between the rotational flows and the sunward flows, while the anticlockwise one is generated from the velocity shear between the tailward flows along the magnetopause and the sunward flows.

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“…This result is consistent with who found a positive correlation with the rate of the deflection and the strength of the magnetic energy density gradient. The intrinsic magnetic polarity of the CME flux rope relative to the background coronal magnetic field determines whether and where the magnetic reconnection can occur and consequently deflects the CME (e.g., see simulation work by Chané et al 2005;Zuccarello et al 2012a;Zhou and Feng 2013). If the CMEs intrinsic field is parallel to the ambient field, the CME deflects equator-ward while when the fields are antiparallel, the CME is likely to deflect poleward (Zhou and Feng 2013).…”

Section: Deflection Dependence On the Background Coronamentioning

confidence: 99%

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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MHD numerical study of the latitudinal deflection of coronal mass ejection

Cited by 33 publications

References 50 publications

Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun

Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun

Modeling the interaction between the solar wind and Saturn's magnetosphere by the AMR‐CESE‐MHD method

The Physical Processes of CME/ICME Evolution

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