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Relevant bibliographies by topics / Solar Filament

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Journal articles

Academic literature on the topic 'Solar Filament'

Author: Grafiati

Published: 4 June 2021

Last updated: 2 February 2022

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Journal articles on the topic "Solar Filament"

1

Schmieder, Brigitte, Guillaume Aulanier, and Tibor Török. "Solar prominences." Proceedings of the International Astronomical Union 4, S257 (2008): 223–32. http://dx.doi.org/10.1017/s1743921309029330.

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AbstractSolar filaments (or prominences) are magnetic structures in the corona. They can be represented by twisted flux ropes in a bipolar magnetic environment. In such models, the dipped field lines of the flux rope carry the filament material and parasitic polarities in the filament channel are responsible for the existence of the lateral feet of prominences.Very simple laws do exist for the chirality of filaments, the so-called “filament chirality rules”: commonly dextral/sinistral filaments corresponding to left- (resp. right) hand magnetic twists are in the North/South hemisphere. Combini

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2

Ambrož, P., and W. Pötzi. "Horizontal flow below solar filaments." Astronomy & Astrophysics 613 (May 2018): A39. http://dx.doi.org/10.1051/0004-6361/201731162.

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Context. Observations of the internal fine structures of solar filaments indicate that the threads of filaments follow magnetic field lines. The magnetic field inside the filament has a strong axial component. Some models of magnetic fields suggest that the field structure in filaments could be caused by the horizontal plasma velocity field near both sides below the filament, where observable shearing effects from the axial component are expected. Aims. The horizontal velocity field in the vicinity of polarity inversion lines is measured in order to determine, if it exhibits a systematic movem

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3

Filippov, Boris. "Filament Connectivity and “Reconnection”." Proceedings of the International Astronomical Union 8, S300 (2013): 412–13. http://dx.doi.org/10.1017/s1743921313011320.

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AbstractStable long lived solar filaments during their lives can approach each other, merge, and form circular structures. Since filaments follow large scale polarity inversion lines of the photospheric magnetic field, their evolution reflects changes of the photospheric field distribution. On the other hand, filament interaction depends on their internal magnetic structure reviled in particular by filament chirality. Possibility of magnetic field line reconnection of neighbor filaments is discussed. Many examples of connectivity changes in a course of photospheric field evolution were found i

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4

Engvold, O. "Cold Matter in Filament Channels." International Astronomical Union Colloquium 144 (1994): 297–308. http://dx.doi.org/10.1017/s0252921100025495.

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AbstractThe formation of cold filaments in the low corona is a central research area in solar physics. Their basic properties are not well understood, but they may be crucial for the mass and magnetic flux balance in the solar corona. The review discusses multi-wavelength observational results and theoretical modelling of filament channels and quiescent filaments.

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5

Martin, S. F., O. Panasenco, O. Engvold, and Y. Lin. "The link between CMEs, filaments and filament channels." Annales Geophysicae 26, no. 10 (2008): 3061–66. http://dx.doi.org/10.5194/angeo-26-3061-2008.

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Abstract. We present a broad concept for the build-up to eruptive solar events which needs to be tested in future observational and theoretical research. In this concept an eruptive solar event consists of a coronal mass ejection, a filament eruption, a cavity around the filament, and a flare. In our picture, the initial energy source must be external to this eruptive system but also feed into it. Among all eruptive events the common denominator is a filament channel with canceling magnetic fields along a primary polarity reversal boundary. We find that magnetic reconnection at or close to the

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6

Aboudarham, J., I. Scholl, N. Fuller, et al. "Automatic detection and tracking of filaments for a solar feature database." Annales Geophysicae 26, no. 2 (2008): 243–48. http://dx.doi.org/10.5194/angeo-26-243-2008.

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Abstract. A new method for the automatic detection and tracking of solar filaments is presented. The method addresses the problems facing existing catalogs, such as the one developed recently in the frame of the European Grid of Solar Observations (EGSO) project. In particular, it takes into account the structural and temporal evolution of filaments, differences in intensity as seen from one observation to the next, and the possibility of sudden disappearance followed by reappearance. In this study, the problem of tracking is solved by plotting all detected filaments during each solar rotation

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7

Ambrož, Pavel, and Alfred Schroll. "Large-scale Motion of Solar Filaments." International Astronomical Union Colloquium 179 (2000): 205–8. http://dx.doi.org/10.1017/s0252921100064502.

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AbstractPrecise measurements of heliographic position of solar filaments were used for determination of the proper motion of solar filaments on the time-scale of days. The filaments have a tendency to make a shaking or waving of the external structure and to make a general movement of whole filament body, coinciding with the transport of the magnetic flux in the photosphere. The velocity scatter of individual measured points is about one order higher than the accuracy of measurements.

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8

Martens, Petrus C., Anthony R. Yeates, and Karthik G. Pillai. "Hemispheric Patterns in Filament Chirality and Sigmoid Shape over the Solar Cycle." Proceedings of the International Astronomical Union 8, S300 (2013): 135–38. http://dx.doi.org/10.1017/s1743921313010867.

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AbstractThe motivation for our research was to study the correlation between the chirality of filaments and the handedness (S- or Z-shape) of sigmoids. It was assumed that sigmoids would mostly coincide with filaments and that the S-shaped sigmoids would correlate well with filaments of sinistral chirality, which we found that to be at best a very weak relation. Since we had a full solar cycle of filament metadata at hand it was easy to verify the supposedly known hemispheric preference of filament chirality. We discovered that the hemispheric chirality rule was confirmed for the epoch where a

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9

Wang, Rui, Ying D. Liu, Ivan Zimovets, Huidong Hu, Xinghua Dai, and Zhongwei Yang. "SYMPATHETIC SOLAR FILAMENT ERUPTIONS." Astrophysical Journal 827, no. 1 (2016): L12. http://dx.doi.org/10.3847/2041-8205/827/1/l12.

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10

Mackay, Duncan H., and Anthony R. Yeates. "Explaining the Hemispheric Pattern of Filament Chirality." Proceedings of the International Astronomical Union 8, S300 (2013): 172–75. http://dx.doi.org/10.1017/s1743921313010934.

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AbstractSolar filaments are known to exhibit a hemispheric pattern in their chirality, where dextral/sinistral filaments dominate in the northern/southern hemisphere. We show that this pattern may be explained through data driven 3D global magnetic field simulations of the Sun's large-scale magnetic field. Through a detailed comparison with 109 filaments over a 6 month period, the model correctly reproduces the filament chirality and helicity with a 96% agreement. The data driven simulation is extended to run over a full solar cycle, where predictions are made for the spatial and temporal depe

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