Results 201 to 210 of about 3,285 (232)

Thin Threads of Solar Filaments

Solar Physics, 2005
High-resolution images obtained in Hα with the new Swedish Solar Telescope at La Palma, Spain, have been used for studies of fine-scale threads in solar filaments. The widths of the thin threads are ≤0.3 arcsec. The fact that the width of the thinnest threads is comparable to the diffraction limit of the telescope of about 0.14 arcsec, at the ...
Yong Lin, OddbjØrn Engvold, Luc Rouppe van der Voort, Jun Elin Wiik, Thomas E. Berger   +4 more
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Solar Filaments and Photospheric Network

Solar Physics, 2005
The locations of barbs of quiescent solar filaments are compared with the photospheric/chromospheric network, which thereby serves as a proxy of regions with enhanced concentrations of magnetic flux. The study covers quiet regions, where also the photospheric network as represented by flow converging regions, i.e., supergranular cell boundaries ...
Yong Lin, Jun Elin Wiik, Oddbjørn Engvold, Luc Rouppe Van Der Voort, Zoe A. Frank   +4 more
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The corona associated with solar filaments

Solar Physics, 1981
Spectroheliograms in high temperature ions such as Fe XV show the existence of both filaments that are brighter than the ambient corona and filaments that are darker than the ambient corona. The relationship of the filaments to photospheric magnetograms is described, and a possible physical mechanism to explain the differences is discussed.
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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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ON the origin of solar filament magnetic fields

Astronomical & Astrophysical Transactions, 1999
Abstract An analysis is made of vector-magnetograms and of the velocity network associated with super-granulation in the photosphere, in the region of a quiescent filament. Observational data were obtained with the Sayan observatory vector-magnetograph.
V. M. Grigoryev, L. V. Ermakova
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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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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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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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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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