Polarimetric Studies of a Fast Coronal Mass Ejection

Mierla, M.; Inhester, B.; Zhukov, A. N.; Shestov, S. V.; Бемпорад, А.; Lamy, Philippe; Koutchmy, S.

doi:10.1007/s11207-022-02018-0

Cited by 3 publications

(3 citation statements)

References 53 publications

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“…(2020), and Mierla et al. (2022), among others, have reported deviations from radial direction that form early in the eruptive process. However, this does not exclude the possibility that the CME may undergo further deflection as it propagates.…”

Section: Discussionmentioning

confidence: 93%

“…A similar number of eruptions fall into each of these two categories, suggesting that the offset in latitude and the correlation between the PEPM and CME offsets in latitude is more likely a result of the local topology and dynamics of the eruptive field than a result of global magnetic structure deflecting the CME toward the equator. Cremades and Bothmer (2004), Liewer et al (2015), Möstl et al (2015), Sahade et al (2020), andMierla et al (2022), among others, have reported deviations from radial direction that form early in the eruptive process. However, this does not exclude the possibility that the CME may undergo further deflection as it propagates.…”

Section: Tablementioning

confidence: 95%

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Partially Erupted Prominence Material as a Diagnostic of Coronal Mass Ejection Trajectory

Hovis‐Afflerbach,

Thompson,

Mason

2023

Space Weather

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Coronal mass ejections (CMEs) are energetic releases of large‐scale magnetic structures from the Sun. CMEs can have impacts on spacecraft and at Earth. This trajectory is typically assumed to be radial, but often the CME moves outward with some spatial offset from the source region where the eruption initially occurred. A CME is frequently accompanied by a prominence eruption, a movement of cool, dense material up into the corona that can be ejected or fall back down. We investigate eruptions in which some portion of the prominence material falls back to the Sun along field lines which have reconfigured in the eruption, rather than draining back to the source or escaping with the CME. Using a method called persistence mapping, 304 Å images from the Solar Dynamics Observatory (SDO), and coronagraph images from the Solar and Heliospheric Observatory, we measure and compare the offsets in latitude of 20 CMEs and their respective prominences with respect to the source region. The 20 events were chosen to sample over the first 10 years of the SDO mission. We find that the offsets are correlated. We find no difference between eruptions offset toward the equator or the poles, suggesting that the offset is a result of local changes in the eruptive field, rather than of the Sun's global magnetic field structure. These findings help us contextualize individual eruptions and highlight changes in the local magnetic field associated with the prominence eruption.

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Section: Discussionmentioning

confidence: 93%

Section: Tablementioning

confidence: 95%

Partially Erupted Prominence Material as a Diagnostic of Coronal Mass Ejection Trajectory

Hovis‐Afflerbach,

Thompson,

Mason

2023

Space Weather

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“…However, current understanding of three-dimensional structure and evolution of CMEs relies primarily on models, because the relevant structures are, in general, oriented by the Sun's rotational axis and the longitudinal view is inaccessible from the ecliptic plane. While some 3-D information about CMEs is available from stereoscopy (Howard et al, 2008;Liewer et al, 2011;Volpes & Bothmer, 2015), polarized imaging (Howard et al, 2013;DeForest et al, 2017;Mierla et al, 2022), or kinematically constrained tomography (Jackson et al, 2011), these methods are limited by line-of-sight effects and cannot alone fully address the east/west structure of CMEs and their interaction with the corona and heliosphere.…”

Section: Introductionmentioning

confidence: 99%

CME Origins and Propagation: Importance of the Polar Perspective

DeForest,

Viall-Kepko,

Fan

et al. 2023

Bulletin of the AAS

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This paper describes the importance of out-of-ecliptic imaging from a polar or nearpolar vantage, to the science of coronal mass ejection origins and propagation. In particular, imaging CMEs from only in or near the ecliptic plane limits understanding of their longitudinal structure and extent, and many other aspects of their formation and propagation including the development and release of the flux ropes that drive the strongest CMEs, and the bidirectional effects between CME propagation and the surrounding corona. Polar-vantage imaging is needed to resolve many current mysteries at the heart of heliophysics. Near-Sun imaging of the magnetic field and coronal EUV emission track interaction between CME onset and the surrounding corona and address outstanding questions of CME formation and early propagation. Coronal and heliospheric polar-vantage imaging is critical to outstanding problems of CME launch, acceleration, evolution, and deflection, which are major sticking points both for solar and heliospheric physics and for the applied science of space weather forecasting.

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