Deflected propagation of a coronal mass ejection from the corona to interplanetary space

Wang, Yuming; Wang, Boyi; Shen, Chenglong; Shen, Fang; Lugaz, Noé

doi:10.1002/2013ja019537

Cited by 94 publications

(76 citation statements)

References 78 publications

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“…The speed, density, pressure, magnetic field, and shock structure can all change as the ICME expands and interacts both with the ambient solar wind as well as with various disturbances within it. In particular, through observational and modeling work, studies have shown that during propagation the flux rope may kink and deform [ Manchester et al , ], reconnection/erosion of internal ICME magnetic flux may occur [ Lavraud et al , ; Ruffenach et al , ], and the ICME may also get deflected [ Manchester et al , ; Kay et al , , ; Wang et al , ] and rotated [ Kliem et al , ; Lynch et al , ]. A recent CME event study by Nieves‐Chinchilla et al [] using both in situ and remote sensing observations from STEREO, SOHO, MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER), and Wind showed evidence for significant reorientation of the flux rope axis.…”

Section: Introductionmentioning

confidence: 99%

Longitudinal conjunction between MESSENGER and STEREO A: Development of ICME complexity through stream interactions

et al. 2016

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We use data on an interplanetary coronal mass ejection (ICME) seen by MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) and STEREO A starting on 29 December 2011 in a near‐perfect longitudinal conjunction (within 3°) to illustrate changes in its structure via interaction with the solar wind in less than 0.6 AU. From force‐free field modeling we infer that the orientation of the underlying flux rope has undergone a rotation of ∼80° in latitude and ∼65° in longitude. Based on both spacecraft measurements as well as ENLIL model simulations of the steady state solar wind, we find that interaction involving magnetic reconnection with corotating structures in the solar wind dramatically alters the ICME magnetic field. In particular, we observed a highly turbulent region with distinct properties within the flux rope at STEREO A, not observed at MESSENGER, which we attribute to interaction between the ICME and a heliospheric plasma sheet/current sheet during propagation. Our case study is a concrete example of a sequence of events that can increase the complexity of ICMEs with heliocentric distance even in the inner heliosphere. The results highlight the need for large‐scale statistical studies of ICME events observed in conjunction at different heliocentric distances to determine how frequently significant changes in flux rope orientation occur during propagation. These results also have significant implications for space weather forecasting and should serve as a caution on using very distant observations to predict the geoeffectiveness of large interplanetary transients.

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Section: Introductionmentioning

confidence: 99%

Longitudinal conjunction between MESSENGER and STEREO A: Development of ICME complexity through stream interactions

et al. 2016

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“…Observations and simulations show that the largest CME deflections and rotations occur in the corona (Byrne et al, ; Isavnin et al, ; Kay, Gopalswamy, Xie, et al, ; Kay, Opher, et al, ), but observations suggest that interplanetary deflections may also occur (e.g., Liu et al, ; Lugaz et al, ; Wang et al, , ). Multiple interplanetary coronal mass ejections (ICMEs) interacting can lead to deflections (e.g., Lugaz et al, , ; Xiong et al, ).…”

Section: Introductionmentioning

confidence: 99%

Using the Coronal Evolution to Successfully Forward Model CMEs' In Situ Magnetic Profiles

Kay

Gopalswamy

2017

JGR Space Physics

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Predicting the effects of a coronal mass ejection (CME) impact requires knowing if impact will occur, which part of the CME impacts, and its magnetic properties. We explore the relation between CME deflections and rotations, which change the position and orientation of a CME, and the resulting magnetic profiles at 1 AU. For 45 STEREO‐era, Earth‐impacting CMEs, we determine the solar source of each CME, reconstruct its coronal position and orientation, and perform a ForeCAT (Forecasting a CME's Altered Trajectory) simulation of the coronal deflection and rotation. From the reconstructed and modeled CME deflections and rotations, we determine the solar cycle variation and correlations with CME properties. We assume no evolution between the outer corona and 1 AU and use the ForeCAT results to drive the ForeCAT In situ Data Observer (FIDO) in situ magnetic field model, allowing for comparisons with ACE and Wind observations. We do not attempt to reproduce the arrival time. On average FIDO reproduces the in situ magnetic field for each vector component with an error equivalent to 35% of the average total magnetic field strength when the total modeled magnetic field is scaled to match the average observed value. Random walk best fits distinguish between ForeCAT's ability to determine FIDO's input parameters and the limitations of the simple flux rope model. These best fits reduce the average error to 30%. The FIDO results are sensitive to changes of order a degree in the CME latitude, longitude, and tilt, suggesting that accurate space weather predictions require accurate measurements of a CME's position and orientation.

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“…Most of previous studies of fitting locally observed MCs simply assumed that MCs propagate radially from the Sun, which means that

{boldv}_{c} \approx v_{X} \overset{boldX}{true}

. However, statistical and case studies of the propagation and geoeffectiveness of CMEs suggested that CME may experience a deflected propagation in interplanetary space [ Wang et al , ; Kilpua et al , ; Rodriguez et al , ; Lugaz , ; Isavnin et al , , ]. It will obviously provide a nonradial component of the linear propagation motion.…”

Section: Introductionmentioning

confidence: 99%

Investigating plasma motion of magnetic clouds at 1 AU through a velocity‐modified cylindrical force‐free flux rope model

et al. 2015

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(2015), Investigating plasma motion of magnetic clouds at 1 AU through a velocity-modified cylindrical force-free flux rope model, J. Geophys. Res. Space Physics, 120, 1543-1565, doi:10.1002 and usually modeled by a flux rope. By assuming the quasi-steady evolution and self-similar expansion, we introduce three types of global motion into a cylindrical force-free flux rope model and developed a new velocity-modified model for MCs. The three types of the global motion are the linear propagating motion away from the Sun, the expanding, and the poloidal motion with respect to the axis of the MC. The model is applied to 72 MCs observed by Wind spacecraft to investigate the properties of the plasma motion of MCs. First, we find that some MCs had a significant propagation velocity perpendicular to the radial direction, suggesting the direct evidence of the CME's deflected propagation and/or rotation in interplanetary space. Second, we confirm the previous results that the expansion speed is correlated with the radial propagation speed and most MCs did not expand self-similarly at 1 AU. In our statistics, about 62%/17% of MCs underwent a underexpansion/overexpansion at 1 AU and the expansion rate is about 0.6 on average. Third, most interestingly, we find that a significant poloidal motion did exist in some MCs. Three speculations about the cause of the poloidal motion are therefore proposed. These findings advance our understanding of the MC's properties at 1 AU and the dynamic evolution of CMEs from the Sun to interplanetary space.

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Deflected propagation of a coronal mass ejection from the corona to interplanetary space

Cited by 94 publications

References 78 publications

Longitudinal conjunction between MESSENGER and STEREO A: Development of ICME complexity through stream interactions

Longitudinal conjunction between MESSENGER and STEREO A: Development of ICME complexity through stream interactions

Using the Coronal Evolution to Successfully Forward Model CMEs' In Situ Magnetic Profiles

Investigating plasma motion of magnetic clouds at 1 AU through a velocity‐modified cylindrical force‐free flux rope model

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