Eruptive Prominences and Their Association with Coronal Mass Ejections

Webb, D. F.

doi:10.1007/978-3-319-10416-4_16

Cited by 22 publications

(13 citation statements)

References 81 publications

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“…Figure 12 demonstrates some characteristic behavior of cavities in the hours leading up to eruption. This may be classified as "cavity activation", and is likely to be related to similar manifestations in quiescent prominences in the hours prior to their eruption (Martin, 2014) as well as pre-eruption behavior of so-called "streamer blowouts" (Webb, 2014). In particular, cavities appear to slowly increase in height, to narrow and become more teardrop-shaped, and to exhibit more sharply defined sub-structure prior to eruption.…”

Section: Open Questionsmentioning

confidence: 98%

Coronal Cavities: Observations and Implications for the Magnetic Environment of Prominences

Gibson

2014

Solar Prominences

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Dark and elliptical, coronal cavities yield important clues to the magnetic structures that cradle prominences, and to the forces that ultimately lead to their eruption. We review observational analyses of cavity morphology, thermal properties (density and temperature), line-of-sight and plane-of-sky flows, substructure including hot cores and central voids, linear polarization signatures, and observational precursors and predictors of eruption. We discuss a magnetohydrodynamic interpretation of these observations which argues that the cavity is a magnetic flux rope, and pose a set of open questions for further study.

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Section: Open Questionsmentioning

confidence: 98%

Coronal Cavities: Observations and Implications for the Magnetic Environment of Prominences

Gibson

2014

Solar Prominences

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“…As described in the previous section, CMEs often exhibit a three-part structure that includes the overlying prominence cavity and embedded filament. A review of CME and prominence eruption associations is provided by Webb (2015). Complementary reviews on prominence eruption dynamics and space weather implications are also provided by Gopalswamy (2015) and Lugaz (2015), respectively.…”

Section: Coronal Mass Ejections (Cmes)mentioning

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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“…Thus, long-term study of prominences over several cycles and at different phases of solar cycle can give valuable insight on the physics of the solar atmosphere. There have been several studies to correlate eruptive prominence distributions and coronal mass ejections (CMEs; Fan, 2015;Gopalswamy et al, 2003;Gopalswamy, 2015;Gilbert et al, 2000;Lugaz, 2015;Schrijver et al, 2008;Webb, 2015). Lockyer, (1908Lockyer, ( , 1922Lockyer, ( , 1931 using coronal drawings and photographs obtained during the total solar eclipse suggested that there is an intimate connection between the distribution of prominences around the solar limb and the forms of corona.…”

Section: Introductionmentioning

confidence: 99%

Time‐Latitude Distribution of Prominences for 10 Solar Cycles: A Study Using Kodaikanal, Meudon, and Kanzelhohe Data

Chatterjee

Hegde

Banerjee

et al. 2020

Earth and Space Science

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Solar prominences are structures of importance because of their role in polar field reversal. We study the long‐term variation of the time latitude distribution of solar prominences in this article. To accomplish this, we primarily used the digitized disc‐blocked Ca II K spectroheliograms as recorded from Kodaikanal Solar Observatory for the period of 1906–2002. For improving the data statistics we included full disc H α images from Meudon and Kanzelhohe Observatory, which are available after 1980. We developed an automated technique to identify the latitudinal locations of prominences in daily images from all three data sets. Derived time‐latitude distribution clearly depicted poleward migration of prominence structures for 10 cycles (15–24). Unlike previous studies, we separated the rate of poleward migration during onset and near pole, using piece‐wise linear fits. In most cases, we found acceleration in poleward migration with the change occurring near ±70° latitudes. The derived migration rates for such large number of solar cycles can provide important inputs toward understanding polar field buildup process.

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Eruptive Prominences and Their Association with Coronal Mass Ejections

Cited by 22 publications

References 81 publications

Coronal Cavities: Observations and Implications for the Magnetic Environment of Prominences

Coronal Cavities: Observations and Implications for the Magnetic Environment of Prominences

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

Time‐Latitude Distribution of Prominences for 10 Solar Cycles: A Study Using Kodaikanal, Meudon, and Kanzelhohe Data

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