Formation and Large-Scale Patterns of Filament Channels and Filaments

Mackay, D. H.

doi:10.1007/978-3-319-10416-4_14

Cited by 19 publications

(11 citation statements)

References 91 publications

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“…Hence, understanding FC formation equates to understanding the pre-eruptive configuration in the corona. FC properties are reviewed in several papers (e.g., Martin, 1998;Mackay, 2015).…”

Section: Filament Channel Formationmentioning

confidence: 99%

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

et al. 2020

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A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multiheight vector magnetic field measurements is the optimal approach for resolving

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“…Hence, understanding FC formation equates to understanding the pre-eruptive configuration in the corona. FC properties are reviewed in several papers (e.g., Martin, 1998;Mackay, 2015).…”

Section: Filament Channel Formationmentioning

confidence: 99%

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

et al. 2020

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“…7a). They are arguably “more fundamental than filaments” (Mackay 2015), since a filament channel may exist without a filament, but a filament cannot exist without a filament channel. The patterns formed by the fibrils as they relate to surrounding magnetic fields has been interpreted as a indication of magnetic chirality, or handedness (Martin 1998a).…”

Section: Beyond Bones: the Prominence In Contextmentioning

confidence: 99%

“…In particular, the abiding presence of a prominence implies a magnetic structure that can provide sustained gravitational support and thermal isolation. Several excellent review chapters within the recent book Solar Prominences (Engvold and Vial 2015) cover our theoretical understanding of the origins of such magnetic structures and their evolution on a variety of temporal and spatial scales (Mackay 2015), the energetic processes associated with prominence formation and visibility (Gilbert 2015; Heinzel 2015; Karpen 2015), and the mechanisms responsible for the ultimate fate of many prominences as the cores of solar eruptions (Fan 2015). Prominence observations and interpretation are also well-covered by other chapters within that book (Ballester 2015; Engvold 2015; Gibson 2015; Gopalswamy 2015; Kucera 2015; Labrosse 2015; López Ariste 2015; Lugaz 2015; Martin 2015; Parenti 2015; Webb 2015) and by the Living Reviews on “Prominence Oscillations” by Arregui et al.…”

Section: Introductionmentioning

confidence: 99%

Solar prominences: theory and models

Gibson

2018

Living Rev Sol Phys

108

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Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observations spanning the solar atmosphere. We obtain the core of this understanding from observations that give us information about the structure of the “magnetic skeleton” that supports and surrounds the prominence. Energetically-sophisticated magnetohydrodynamic simulations then add flesh and blood to the skeleton, demonstrating how a thermally varying plasma may pulse through to form the prominence, and how the plasma and magnetic fields dynamically interact.

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“…Cavities are commonly modeled as magnetic flux ropes (e.g. Low and Hundhausen 1995;Fan 2012) and may be inherent components of filament systems that form from helicity accumulation (Mackay, 2015). At least a third of cavities erupt (Forland et al, 2013), though many of those that do not may simply erupt sometime after they were observed at the limb.…”

Section: Cavitymentioning

confidence: 99%

Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog

et al. 2015

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We present a statistical study of prominence and filament eruptions observed by the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO). Several properties are recorded for 904 events that were culled from the Heliophysics Event Knowledgebase (HEK) and incorporated into an online catalog for general use. These characteristics include the filament and eruption type, eruption symmetry and direction, apparent twisting and writhing motions, and the presence of vertical threads and coronal cavities. Associated flares and white-light coronal mass ejections (CME) are also recorded. Total rates are given for each property along with how they differ among filament types. We also examine the kinematics of 106 limb events to characterize the distinct slow-and fast-rise phases often exhibited by filament eruptions. The average fast-rise onset height, slow-rise duration, slow-rise velocity, maximum field-of-view (FOV) velocity, and maximum FOV acceleration are 83 Mm, 4.4 hours, 2.1 km s -1 , 106 km s -1 , and 111 m s -2 , respectively. All parameters exhibit lognormal probability distributions similar to that of CME speeds. A positive correlation between latitude and fast-rise onset height is found, which we attribute to a corresponding negative correlation in the average vertical magnetic field gradient, or decay index, estimated from potential field source surface (PFSS) extrapolations. We also find the decay index at the fast-rise onset point to be 1.1 on average, consistent with the critical instability threshold theorized for straight current channels. Finally, we explore relationships between the derived kinematics properties and apparent twisting motions. We find that events with evident twist have significantly faster CME speeds and significantly lower fast-rise onset heights, suggesting relationships between these values and flux rope helicity.

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Formation and Large-Scale Patterns of Filament Channels and Filaments

Cited by 19 publications

References 91 publications

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections

Solar prominences: theory and models

Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog

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