The Deflection of Coronal Mass Ejections by the Ambient Coronal Magnetic Field Configuration

Wang, Jingjing; Hoeksema, J. T.; Liu, Siqing

doi:10.1029/2019ja027530

Cited by 11 publications

(12 citation statements)

References 64 publications

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“…The CME is therefore likely to be influenced by B 2 present in the surrounding potential field, in agreement with previous studies (Gui et al 2011;Kay et al 2013;Sieyra et al 2001, and references therein) and to be deflected southward contrary to the general equatorial deflection of many CMEs (Cremades & Bothmer 2004). The presence of open field lines, deflected toward the south, is also expected to deflect the CME along them (Mäkelä et al 2013;Wang et al 2020, and references therein).…”

Section: Global Magnetic Field Modelsupporting

confidence: 88%

The Magnetic Environment of a Stealth Coronal Mass Ejection

O’Kane¹,

Cormack

Mandrini

et al. 2021

ApJ

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Interest in stealth coronal mass ejections (CMEs) is increasing due to their relatively high occurrence rate and space weather impact. However, typical CME signatures such as extreme-ultraviolet dimmings and post-eruptive arcades are hard to identify and require extensive image processing techniques. These weak observational signatures mean that little is currently understood about the physics of these events. We present an extensive study of the magnetic field configuration in which the stealth CME of 2011 March 3 occurred. Three distinct episodes of flare ribbon formation are observed in the stealth CME source active region (AR). Two occurred prior to the eruption and suggest the occurrence of magnetic reconnection that builds the structure that will become eruptive. The third occurs in a time close to the eruption of a cavity that is observed in STEREO-B 171 Å data; this subsequently becomes part of the propagating CME observed in coronagraph data. We use both local (Cartesian) and global (spherical) models of the coronal magnetic field, which are complemented and verified by the observational analysis. We find evidence of a coronal null point, with field lines computed from its neighborhood connecting the stealth CME source region to two ARs in the northern hemisphere. We conclude that reconnection at the null point aids the eruption of the stealth CME by removing the field that acted to stabilize the preeruptive structure. This stealth CME, despite its weak signatures, has the main characteristics of other CMEs, and its eruption is driven by similar mechanisms.

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Section: Global Magnetic Field Modelsupporting

confidence: 88%

The Magnetic Environment of a Stealth Coronal Mass Ejection

O’Kane¹,

Cormack

Mandrini

et al. 2021

ApJ

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“…Moving further, we also found that the CME deflected away from radial direction, most likely after the aforesaid interaction. Such CMEs provide useful reference for space weather forecasting, especially for CME arrival and geoeffectiveness (Wang et al 2020). This suggests a possible working hypothesis for a future research, i.e.…”

Section: Discussionmentioning

confidence: 83%

Solar Coronal Density Turbulence and Magnetic Field Strength at the Source Regions of Two Successive Metric Type II Radio Bursts

Ramesh

Kathiravan

Kumari

2023

ApJ

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We report spectral and polarimeter observations of two weak, low-frequency (≈85–60 MHz) solar coronal type II radio bursts that occurred on 2020 May 29 within a time interval ≈2 minutes. The bursts had fine structures, and were due to harmonic plasma emission. Our analysis indicates that the magnetohydrodynamic shocks responsible for the first and second type II bursts were generated by the leading edge (LE) of an extreme-ultraviolet flux rope/coronal mass ejection (CME) and interaction of its flank with a neighboring coronal structure, respectively. The CME deflected from the radial direction by ≈25° during propagation in the near-Sun corona. The estimated power spectral density and magnetic field strength (B) near the location of the first burst at heliocentric distance r ≈ 1.35 R ⊙ are ≈2 × 10−3 W2m and ≈1.8 G, respectively. The corresponding values for the second burst at the same r are ≈10−3 W2m and ≈0.9 G. The significant spatial scales of the coronal turbulence at the location of the two type II bursts are ≈62–1 Mm. Our conclusions from the present work are that the turbulence and magnetic field strength in the coronal region near the CME LE are higher compared to the corresponding values close to its flank. The derived estimates of the two parameters correspond to the same r for both the CME LE and its flank, with a delay of ≈2 minutes for the latter.

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“…It is generally accepted that neighboring magnetic structures, such as coronal holes (CHs -e.g., Cremades et al 2006;Gopalswamy et al 2009;Sahade et al 2020Sahade et al , 2021 and active regions (ARs -e.g., Kay et al 2015;Möstl et al 2015;Wang et al 2015), can deflect MFRs in longitude and latitude against their position. On the other hand, heliospheric current sheets (e.g., Liewer et al 2015;Wang et al 2020), helmet-streamers (e.g., Zuccarello et al 2012;Yang et al 2018), and pseudostreamers (PSs -e.g., Cécere et al 2020;Wang et al 2020;Karna et al 2021;Sahade et al 2022) attract MFRs toward their low magnetic field regions. This responses can be quantified, in strength and direction, by the local and global gradients of the magnetic pressure (Gui et al 2011;Panasenco et al 2013;Liewer et al 2015;Sieyra et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Understanding the deflection of the `Cartwheel CME': data analysis and modeling

Sahade¹,

Vourildas²,

Balmaceda³

et al. 2023

Preprint

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We study the low corona evolution of the 'Cartwheel' coronal mass ejection (CME; 2008-04-09) by reconstructing its 3D path and modeling it with magneto-hydrodynamic simulations. This event exhibits a double-deflection that has been reported and analyzed in previous works but whose underlying cause remained unclear. The 'Cartwheel CME' travels toward a coronal hole (CH) and against the magnetic gradients. Using a high-cadence, full trajectory reconstruction, we accurately determine the location of the magnetic flux rope (MFR) and, consequently, the magnetic environment in which it is immersed. We find a pseudostreamer (PS) structure whose null point may be responsible for the complex evolution of the MFR at the initial phase. From the pre-eruptive magnetic field reconstruction, we estimate the dynamic forces acting on the MFR and provide a new physical insight on the motion exhibited by the 2008-04-09 event. By setting up a similar magnetic configuration in a 2.5D numerical simulation we are able to reproduce the observed behavior, confirming the importance of the PS null point. We find that the magnetic forces directed toward the null point cause the first deflection, directing the MFR towards the CH. Later, the magnetic pressure gradient of the CH produces the reversal motion of the MFR.

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The Deflection of Coronal Mass Ejections by the Ambient Coronal Magnetic Field Configuration

Cited by 11 publications

References 64 publications

The Magnetic Environment of a Stealth Coronal Mass Ejection

The Magnetic Environment of a Stealth Coronal Mass Ejection

Solar Coronal Density Turbulence and Magnetic Field Strength at the Source Regions of Two Successive Metric Type II Radio Bursts

Understanding the deflection of the `Cartwheel CME': data analysis and modeling

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