Results 261 to 270 of about 4,310 (287)

Various Barbs in Solar Filaments

Publications of the Astronomical Society of Australia, 2017
AbstractInterest to lateral details of the solar filament shape named barbs, motivated by their relationship to filament chirality and helicity, showed their different orientation relative to the expected direction of the magnetic field. While the majority of barbs are stretched along the field, some barbs seem to be transversal to it and are referred ...
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Material ejecta in a disturbed solar filament

Solar Physics, 1987
Hα observations, using the Multichannel Subtractive Double Pass (MSDP) spectrograph operating on the Meudon Solar Tower, have been made of an active region filament which undergoes a ‘disparition brusque’. The period of observation was from 10 ∶ 45 to 13 ∶ 30 UT on 22 June, 1981. Velocity and intensity fluctuations in Hα were measured.
M. A. Raadu, J. M. Malherbe, B. Schmieder, P. Mein   +3 more
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The twisting of filament that resulted in a solar flare

Chinese Astronomy and Astrophysics, 1994
Abstract Based mainly on filtergrams ofHα line center and various offbands and supplemented with measurements of the CIV 1548 line, we analyzed the evolution of a filament during a period of 15 minutes prior to the eruption of the flare of 1980 June 25 in the active region AR 2522.
Lin Yuan-zhang, V. Gaizauskas
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Differential rotation of solar filaments

Solar Physics, 1974
The latitudinal component of solar differential rotation and the possibility of a radial component are discussed and compared to the observed rotational velocities of solar filaments. The author's values of rotational rate versus heliographic latitude for 100 points in the solar atmosphere derived from 17 quiescent filaments are shown to be comparable
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Activated solar filaments and flares

Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences, 1980
Abstract Activations and disruptions of dark Ha filaments are very common phenomena on the Sun. They precede the most powerful two-ribbon solar flares, but they also appear far from any active region without any chromospheric flaring.
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The Dynamics of Solar Filament Channels

2017
This research seeks to expand understanding of the processes which occur in solar filament channels by both modeling and observational methods. Firstly, a cutting-edge area of Non-Linear Force Free modeling is significantly expanded to allow 3D multiwavelength models with 45 second cadence; this allows prediction of rapid changes to the structures ...
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Differential Rotation of Solar Filaments Early Observed by the OGAUC in the Period 1929 – 1941

Solar Physics, 2022
Miao Wan, K J Li
exaly  

Improvement in the energy conversion efficiency for silicon heterojunction solar cells due to SiOx inserted with conducting filaments

Journal of Alloys and Compounds, 2023
Doowon Lee, Hee-Dong Kim
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 been
Gwangson Choe, Minseon Lee, Sibaek Yi
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Chirality of Solar Filaments and the Supporting Magnetic Field

Geophysical Monograph Series, 2023
P F Chen
exaly