Analysis of Large Deflections of Prominence–CME Events during the Rising Phase of Solar Cycle 24

Sieyra, M. V.; Cécere, M.; Cremades, H.; Iglesias, F. A.; Sahade, Abril; Mierla, M.; Stenborg, G.; Costa, Andrea; West, Matthew J.; D’Huys, Elke

doi:10.1007/s11207-020-01694-0

Cited by 17 publications

(22 citation statements)

References 63 publications

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“…While coronal holes (e.g., Cremades et al 2006;Gopalswamy et al 2009;Sahade et al 2020Sahade et al , 2021 and active regions (e.g., Kay et al 2015;Möstl et al 2015;Wang et al 2015) deflect FRs against their location, 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., Bi et al 2013;Wang 2015;Cécere et al 2020;Wang et al 2020) attract FRs to their low magnetic energy regions. Combined effects of the several structures at different heights can be seen in, for example, Sieyra et al (2020). In previous studies (Sahade et al 2020(Sahade et al , 2021, we found that the presence of a coronal hole nearby the eruptive region forms a magnetic null point that attracts the FR.…”

Section: Introductionmentioning

confidence: 68%

Pseudostreamer influence on flux rope evolution

Sahade

Cécere

Sieyra

et al. 2022

A&A

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Context.A highly important aspect of solar activity is the coupling between eruptions and the surrounding coronal magnetic field topology, which determines the trajectory and morphology of the event. Pseudostreamers (PSs) are coronal magnetic structures formed by arcs of twin loops capped by magnetic field lines from coronal holes of the same polarity that meet at a central spine. They contain a single magnetic null point in the spine, just above the closed field lines, which potentially influences the evolution of nearby flux ropes (FRs). Aims. Because of the impact of magnetic FR eruptions on space weather, we aim to improve current understanding on the deflection of CMEs. To understand the net effect of the PS on FR eruptions is first necessary to study diverse and isolated FR-PS scenarios, which are not influenced by other magnetic structures. Methods. We performed numerical simulations in which a FR structure is in the vicinity of a PS magnetic configuration. The combined magnetic field of the PS and the FR results in the formation of two magnetic null points. We evolve this scenario by numerically solving the magnetohydrodynamic equations in 2.5D. The simulations consider a fully ionised compressible ideal plasma in the presence of a gravitational field and a stratified atmosphere. Results. We find that the dynamic behaviour of the FR can be categorised into three different classes based on the FR trajectories and whether it is eruptive or confined. Our analysis indicates that the magnetic null points are decisive in the direction and intensity of the FR deflection and their hierarchy depends on the topological arrangement of the scenario. Moreover, the PS lobe acts as a magnetic cage enclosing the FR. We report that the total unsigned magnetic flux of the cage is a key parameter defining whether the FR is ejected or not.

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Section: Introductionmentioning

confidence: 68%

Pseudostreamer influence on flux rope evolution

Sahade

Cécere

Sieyra

et al. 2022

A&A

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“…Jiang et al (2007) described an event where a CME evolves toward a CH and then moves away from it. Also, in Sieyra et al (2020) (see their figure 14) we found that the trajectory is not always deflected away from the CH but, at low coronal heights, the eruption occasionally approaches the CH, even when the followed path is not directed toward the minimum magnetic energy region. Yang et al (2018) studied the interaction of a small filament with non-CH open field lines.…”

Section: Introductionmentioning

confidence: 71%

“…Many studies suggest that open magnetic fluxes behave as "magnetic walls" that push CMEs away (e.g., Cremades et al 2006;Gopalswamy et al 2009;Gui et al 2011;Cécere et al 2020). However, there are few reported events where the eruptions first get closer to open magnetic fluxes and then move away (Jiang et al 2007;Yang et al 2018;Sieyra et al 2020). In these observational cases the CME structure is close to not only a CH but also other magnetic structures, such as an active region or a pseudostreamer, making it difficult to distinguish which of all the structures are responsible for the double deflection.…”

Section: Discussionmentioning

confidence: 99%

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Polarity relevance in flux rope deflections triggered by coronal holes

Sahade,

Cécere,

Costa

et al. 2021

Preprint

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Context. Many observations show that coronal holes (CHs) deviate coronal mass ejections (CMEs) away from them. However, there are some peculiar events reported where the opposite occurs. Aims. To contribute to a space weather forecast efforts, in relation to the prediction of CME trajectories, we study the interaction between flux ropes (FRs) and CHs through numerical simulations. Methods. We perform 2.5D numerical simulations where FRs and CHs interact with different relative polarity configurations. We also reconstruct the trajectory and magnetic environment of a peculiar event occurred on 30 April 2012. Results. The numerical simulations indicate that at low coronal levels, depending on the relative magnetic field polarity between the FR and the CH, the deflection will be attractive, i.e. the FR moves towards the CH (for anti-aligned polarities) or repulsive, i.e. the FR moves away to the CH (for aligned polarities). This is likely due to the formation of vanishing magnetic field regions or null points, located between the FR and the CH or, at the other side of the FR, respectively. The analysed observational event shows a double-deflection, first departing from the radial direction by approaching the CH and then moving away from it suggesting that the trajectory could result from a magnetic configuration with an anti-aligned polarity. We numerically reproduce the double deflection of the observed event, providing support to this conjecture.

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“…This reconnection process will result in the set of two red field lines representing the transequatorial loops discussed in Section 3.4. Sieyra et al 2020, and references therein) and be deflected southward contrary to the general equatorial deflection of many CMEs (Cremades and Bothmer 2004). The presence of open field lines, deflected towards 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 Modelmentioning

confidence: 98%

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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Analysis of Large Deflections of Prominence–CME Events during the Rising Phase of Solar Cycle 24

Cited by 17 publications

References 63 publications

Pseudostreamer influence on flux rope evolution

Pseudostreamer influence on flux rope evolution

Polarity relevance in flux rope deflections triggered by coronal holes

The Magnetic Environment of a Stealth Coronal Mass Ejection

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