Results 11 to 20 of about 1,095,612 (284)
Proper Motion of Solar Filaments [PDF]
Astronomy & Astrophysics, 1999 Precise measurements of heliographic position of solar filaments were used for describing the proper motion of solar filaments on the time-scale of one day. Only the velocity values more accurate than 100 m s−1 were used for the study. The filaments have a tendency to make a shaking or waving of the external structure and also to make a general ...
P. Ambrož, A. Schroll
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CHIRALITY AND MAGNETIC CONFIGURATIONS OF SOLAR FILAMENTS [PDF]
The Astrophysical Journal, 2017 ABSTRACT It has been revealed that the magnetic topology in the solar atmosphere displays hemispheric preference, i.e., helicity is mainly negative/positive in the northern/southern hemispheres, respectively. However, the strength of the hemispheric rule and its cyclic variation are controversial.
Y. Ouyang (欧阳雨) +3 more
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Developing an Automated Detection, Tracking, and Analysis Method for Solar Filaments Observed by CHASE via Machine Learning [PDF]
The Astrophysical JournalStudies on the dynamics of solar filaments have significant implications for understanding their formation, evolution, and eruption, which are of great importance for space weather warning and forecasting.
Z. Zheng +5 more
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A Breakout Model for Solar Coronal Jets with Filaments [PDF]
The Astrophysical Journal, 2018 Abstract Recent observations have revealed that many solar coronal jets involve the eruption of miniature versions of large-scale filaments. Such “mini-filaments” are observed to form along the polarity inversion lines of strong, magnetically bipolar regions embedded in open (or distantly closing) unipolar field. During the generation of
P. F. Wyper +2 more
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The Connection Between Solar Coronal Cavities And Solar Filaments
, 2017 This project has been supported by funding from the Division of Advanced Cyberinfrastructure within the Directorate for Computer and Information Science and Engineering, the Division of As- tronomical Sciences within the Directorate for Mathematical and Physical Sciences, and the Division of Atmospheric and Geospace Sciences within the Directorate for ...
Zawadzki, Brianna (5588942) +1 more
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Falling Threads during Solar Filament Eruptions
The Astrophysical JournalMass drainage is frequently observed in solar filaments. During filament eruptions, falling material most likely flows along magnetic field lines, which may provide important clues for the magnetic structures of filaments.
Yidian Wu +3 more
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On the Fine Structure of Solar Filaments [PDF]
The Astrophysical Journal, 2006 High-resolution Hα images of solar filaments show a variety of dark fine-structure fibrils, most of them aligned with the magnetic field that is sheared with respect to the filament long axis. Here we demonstrate how such fibrils can be explained in terms of the magnetic field dips produced by realistic mass loading due to plasma condensation along the
Heinzel, P., Anzer, U.
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SWAYING THREADS OF A SOLAR FILAMENT [PDF]
The Astrophysical Journal, 2009 From recent high resolution observations obtained with the Swedish 1 m Solar Telescope in La Palma, we detect swaying motions of individual filament threads in the plane of the sky. The oscillatory character of these motions are comparable with oscillatory Doppler signals obtained from corresponding filament threads.
Lin, Y. +6 more
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SOLAR MAGNETIZED “TORNADOES:” RELATION TO FILAMENTS [PDF]
The Astrophysical Journal, 2012 Solar magnetized "tornadoes", a phenomenon discovered in the solar atmosphere, appear as tornado-like structures in the corona but root in the photosphere. Like other solar phenomena, solar tornadoes are a feature of magnetized plasma and therefore differ distinctly from terrestrial tornadoes. Here we report the first analysis of solar "tornadoes" {Two
Yang Su +4 more
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Where Do Solar Filaments Form? [PDF]
Proceedings of the International Astronomical Union, 2013 AbstractIn the present study, we consider where large, stable solar filaments form relative to underlying magnetic polarities. We find that 92% of all large stable filaments form in magnetic configurations involving the interaction of two or more bipoles. Only 7% form above the Polarity Inversion Line (PIL) of a single bipole. This indicates that a key
Mackay, Duncan H. +2 more
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