Origins of Rolling, Twisting, and Non-radial Propagation of Eruptive Solar Events

Martin, Sara; Panasenco, O.

doi:10.1007/978-1-4899-8005-2_24

Cited by 9 publications

(11 citation statements)

References 12 publications

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“…Defining the background is one of the key inputs needed for understanding CME propagation (see e.g., Roussev et al 2012;Arge et al 2013). However, there are other processes that can significantly affect the propagation of CMEs: CME-CME interaction (see e.g., Gopalswamy et al 2001a;2012c;Temmer et al 2012;Harrison et al 2012;Lugaz et al 2012;Liu et al 2014a;Sterling et al 2014;Temmer et al 2014) and CME deflection by largescale structures such as coronal holes and streamers (Gopalswamy 2010(Gopalswamy , 2009dShen et al 2011;Gui et al 2011;Wood et al 2012;Kay et al 2013;Panasenco et al 2013;Gopalswamy and Mäkelä 2014).…”

Section: Propagation Effects: Deflection Interaction and Rotation Omentioning

confidence: 99%

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Gopalswamy

Tsurutani

Yan

2015

Prog. in Earth and Planet. Sci.

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This paper presents an overview of results obtained during the CAWSES-II period on the short-term variability of the Sun and how it affects the near-Earth space environment. CAWSES-II was planned to examine the behavior of the solar-terrestrial system as the solar activity climbed to its maximum phase in solar cycle 24. After a deep minimum following cycle 23, the Sun climbed to a very weak maximum in terms of the sunspot number in cycle 24 (MiniMax24), so many of the results presented here refer to this weak activity in comparison with cycle 23. The short-term variability that has immediate consequence to Earth and geospace manifests as solar eruptions from closed-field regions and high-speed streams from coronal holes. Both electromagnetic (flares) and mass emissions (coronal mass ejections -CMEs) are involved in solar eruptions, while coronal holes result in high-speed streams that collide with slow wind forming the so-called corotating interaction regions (CIRs). Fast CMEs affect Earth via leading shocks accelerating energetic particles and creating large geomagnetic storms. CIRs and their trailing high-speed streams (HSSs), on the other hand, are responsible for recurrent small geomagnetic storms and extended days of auroral zone activity, respectively. The latter leads to the acceleration of relativistic magnetospheric 'killer' electrons. One of the major consequences of the weak solar activity is the altered physical state of the heliosphere that has serious implications for the shock-driving and storm-causing properties of CMEs. Finally, a discussion is presented on extreme space weather events prompted by the 23 July 2012 super storm event that occurred on the backside of the Sun. Many of these studies were enabled by the simultaneous availability of remote sensing and in situ observations from multiple vantage points with respect to the Sun-Earth line.

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Section: Propagation Effects: Deflection Interaction and Rotation Omentioning

confidence: 99%

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Gopalswamy

Tsurutani

Yan

2015

Prog. in Earth and Planet. Sci.

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“…However, the island formation and ejection from the reconnection region is highly dynamic and both our results and the Karpen et al (2012) simulations show the islands are both continually moving out of the way of the erupting CME and are much much smaller than the CME flux ropes. Panasenco et al (2012) discussed observations of eruptions from pseudostreamer topologies, including the sympathetic eruptions on 1 August 2010 simulated by Török et al (2011). The deflection (i.e., non-radial propagation) of the prominence material in the early phases of eruption were quantified and showed, at least in some cases, the low coronal trajectories are consistent with being "guided towards weaker field regions, namely null points existing at different heights in the overlying configuration."…”

Section: Cme Deflection During Eruptionmentioning

confidence: 99%

Sympathetic Magnetic Breakout Coronal Mass Ejections From Pseudostreamers

Lynch

Edmondson

2013

ApJ

106

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We present high resolution 2.5-dimensional MHD simulation results of magnetic breakout-initiated coronal mass ejections (CMEs) originating from a coronal pseudostreamer configuration. The coronal null point in the magnetic topology of pseudostreamers means the initiation of consecutive sympathetic eruptions is a natural consequence of the system's evolution. A generic source region energization process -ideal footpoint shearing parallel to the pseudostreamer arcade polarity inversion lines -is all that is necessary to store sufficient magnetic energy to power consecutive CME eruptions given that the pseudostreamer topology enables the breakout initiation mechanism. The second CME occurs because the eruptive flare reconnection of the first CME simultaneously acts as the overlying pre-eruption breakout reconnection for the sympathetic eruption. We examine the details of the magnetic and kinetic energy evolution and the signatures of the overlying null point distortion, current sheet formation, and magnetic breakout reconnection giving rise to the runaway expansion that drives the flare reconnection below the erupting sheared field core. The numerical simulation's spatial resolution and output cadence are sufficient to resolve the formation of magnetic islands during the reconnection process in both the breakout and eruptive flare current sheets. We quantify the flux transfer between the pseudostreamer arcades and show the eruptive flare reconnection processes flux ∼10 times faster than the pre-eruption breakout reconnection. We show that the breakout reconnection jets cause bursty, intermittent upflows along the pseudostreamer stalk as well as downflows in the adjacent pseudostreamer arcade, both of which may be observable as pre-eruption signatures. Finally, we examine the flux rope CME -2trajectories and show that the breakout current sheet provides a path of least resistance as an imbalance in the surrounding magnetic energy density and results in a non-radial CME deflection early in the eruption.

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“…We note that the heliospheric current sheet (HCS) typically lies near the equator at solar minimum, and the dominant coronal holes (CHs) are at the poles. The global magnetic patterns surrounding the source location were suggested to lead to the near‐Sun CME deflections (i.e., Filippov, 2019; Gopalswamy, Mäkelä, et al., 2009; Gui et al., 2011; Kay et al., 2017; Liewer et al., 2015; McCauley et al., 2015; Panasenco et al., 2013); this was also supported by several theoretical studies (i.e., Kliem et al., 2013; Lynch & Edmondson, 2013; Török et al., 2018; Wang & Hess, 2018). For example, Gopalswamy, Mäkelä, et al.…”

Section: Introductionmentioning

confidence: 99%

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

2020

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Solar coronal mass ejections (CMEs) are sometimes deflected during their propagation. This deflection may be the consequence of an interaction between the CME and the ambient coronal field, for example, a coronal hole, or the solar wind. The coronal magnetic field configuration is computed from daily synoptic maps of magnetic field from SOHO/MDI and SDO/HMI using a Potential Field Source Surface model. We analyze 30 halo‐CMEs whose deflection angle exceeds 90° by comparing the ambient magnetic field configuration and the measurement position angles of the CMEs. We find that the deflection of 87% of the CMEs (26 of 30) is consistent with the ambient magnetic field configuration, agreeing with previous studies. Of these 26, 69% are deflected toward the heliospheric current sheet, the boundary between the magnetic field polarities, and 31% toward a pseudo‐streamer, the boundary between same‐polarity magnetic field regions. This implies that the ambient coronal magnetic field configuration plays an important role in the deflection of CMEs and that the current sheet configuration is more important than a pseudo‐streamer. Of the 26 CMEs, the average and standard deviation of the minimum values of the deflection angle in three dimensions relative to an initially radial trajectory are 28° and 14°, respectively.

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Origins of Rolling, Twisting, and Non-radial Propagation of Eruptive Solar Events

Cited by 9 publications

References 12 publications

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Sympathetic Magnetic Breakout Coronal Mass Ejections From Pseudostreamers

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

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