Solar prominences: theory and models

Gibson, S. E.

doi:10.1007/s41116-018-0016-2

Cited by 108 publications

(82 citation statements)

References 202 publications

(262 reference statements)

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“…Note also that in our event, the filament itself did not seem to reach the location of the green circle as the field lines in Figure 6 do. The filament itself likely does not represent the entirety of the erupting flux rope, since filaments are only located in the lower, dipped portions of long, flat, sheared, or twisted field lines (e.g., Gibson & Fan 2006;Dudík et al 2008;Luna et al 2012;Zuccarello et al 2016;Xia & Keppens 2016;Gibson 2018;Gunár et al 2018), while the rest of the flux rope may not be readily apparent in observations. However, as the green circle is located in a coronal dimming region (compare Figure 2a with 4d), the corresponding coronal loop likely reconnected with a flux rope field line not made visible in observations by absorbing filament plasma.…”

Section: Reconnection Of Overlying Coronal Loopsmentioning

confidence: 99%

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Dudík

Lörinčík

Aulanier

et al. 2019

ApJ

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We report on observations of the two newly-identified reconnection geometries involving erupting flux ropes. In 3D, a flux rope can reconnect either with a surrounding coronal arcade (recently named "ar-rf" reconnection) or with itself ("rr-rf" reconnection), and both kinds of reconnection create a new flux rope field line and a flare loop. For the first time, we identify all four constituents of both reconnections in a solar eruptive event, the filament eruption of 2011 June 07 observed by SDO/AIA. The ar-rf reconnection manifests itself as shift of one leg of the filament by more than 25 northward. At its previous location, a flare arcade is formed, while the new location of the filament leg previously corresponded to a footpoint of a coronal loop in 171Å. In addition, the evolution of the flare ribbon hooks is also consistent with the occurrence of ar-rf reconnection as predicted by MHD simulations. Specifically, the growing hook sweeps footpoints of preeruptive coronal arcades, and these locations become inside the hook. Furthermore, the rr-rf reconnection occurs during the peak phase above the flare arcade, in an apparently X-type geometry involving a pair of converging bright filament strands in the erupting filament. A new flare loop forms near the leg of one of the strands, while a bright blob, representing a remnant of the same strand, is seen ascending into the erupting filament. All together, these observations vindicate recent predictions of the 3D standard solar flare model.

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Section: Reconnection Of Overlying Coronal Loopsmentioning

confidence: 99%

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Dudík

Lörinčík

Aulanier

et al. 2019

ApJ

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“…Kuckein et al (2009Kuckein et al ( , 2012b studied an active region filament observed in July, 2005, and suggested a flux rope topology. Together, the field strengths and angles can be used to distinguish between the multiple topologies that were suggested to be able to support the filament plasma, such as the sheared arcade model and the flux rope model (Gibson 2018).…”

Section: Introductionmentioning

confidence: 99%

Magnetic Structure of an Erupting Filament

Wang

Jenkins

Pillet

et al. 2020

ApJ

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The full 3-D vector magnetic field of a solar filament prior to eruption is presented. The filament was observed with the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope in the chromospheric He i line at 10830Å on May 29 and 30, 2017. We inverted the spectropolarimetric observations with the HAnle and ZEeman Light (HAZEL) code to obtain the chromospheric magnetic field. A bimodal distribution of field strength was found in or near the filament. The average field strength was 24 Gauss, but prior to the eruption we find the 90th percentile of field strength was 435 Gauss for the observations on May 29. The field inclination was about 67 degree from the solar vertical. The field azimuth made an angle of about 47 to 65 degree to the spine axis. The results suggest an inverse configuration indicative of a flux rope topology. He i intensity threads were found to be co-aligned with the magnetic field direction. The filament had a sinistral configuration as expected for the southern hemisphere. The filament was stable on May 29, 2017 and started to rise during two observations on May 30, before erupting and causing a minor coronal mass ejection. There was no obvious change of the magnetic topology during the eruption process. Such information on the magnetic topology of erupting filaments could improve the prediction of the geoeffectiveness of solar storms.

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“…Prominences/filaments are structures formed in the solar atmosphere following magnetic polarity inversion lines. They are formed in the chromosphere by cool dense (hundred times cooler and denser than the coronal material) plasma held in place by solar magnetic fields (Engvold, 2015;Gibson, 2018;Martin, 2015). At the limb they appear as bright features when observed in few optical, extreme ultraviolet lines such as H , Ca ii K, and He ii 304 Å.…”

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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Solar prominences: theory and models

Cited by 108 publications

References 202 publications

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Magnetic Structure of an Erupting Filament

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

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