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Differential Rotation of Solar Filaments Early Observed by the OGAUC in the Period 1929 – 1941
Solar Physics, 2022Kejun Li, Miao Wan
exaly
A Clue to the Filamentary Nature of Solar Filaments
It is generally accepted that solar prominences, also known as filaments, are formed through thermal condensation instability from hot coronal plasmas. Within solar prominences (filaments), counter-streaming subscale flows are frequently observed. It is quite surprising that thermal instability in magnetized plasmas with such shear flows has never beenGwangson Choe, Minseon Lee, Sibaek Yi
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Chirality of Solar Filaments and the Supporting Magnetic Field
Geophysical Monograph Series, 2023Peng-Fei Chen
exaly
Tilt Angles of Solar Filaments over the Period of 1919 – 2014
Solar Physics, 2016Andrey Tlatov, Tlatov Andrey G
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Basic magnetic field configurations for solar filament channels and filaments
1997The three-dimensional magnetic structure of solar filament channels and filaments is considered. A simple analytical potential model of a filament channel is setup with line sources representing the overlying arcades and point sources the flux of the filament. A possible explanation of the distinct upper and lower bounds of a filament is given.
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Non-linear analysis of the long-term behaviour of solar filaments
Monthly Notices of the Royal Astronomical Society, 2014Nan Wu
exaly