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Differential rotation of short-lived solar filaments [PDF]
Solar Physics, 1977 We have measured the rotation rate of short-lived solar filaments as a function of their latitude. The resulting rotation curve appears to be somewhat flatter than the corresponding curve for long-lived ...
Frances Tang
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Large-scale motion of solar filaments
Journal of Astrophysics and Astronomy, 2000AbstractPrecise 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 ...
Pavel Ambrož, Alfred Schroll
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Activity cycle of solar filaments
Journal of Astrophysics and Astronomy, 2007Long-term variation in the distribution of the solar filaments observed at the Observatorie de Paris, Section de Meudon from March 1919 to December 1989 is presented to compare with sunspot cycle and to study the periodicity in the filament activity, namely the periods of the coronal activity with the Morlet wavelet used.
K. J. Li +5 more
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1966
Abstract : A survey was made of the Lockheed solar patrol films in search of any parameters which could possible be linked with the occurrence of flares. High resolution observations ( or = 1 sec of arc) show that some filaments increase in darkness and become more sharply defined within several hours to several days before the onset of a flare ...
Sara F. Smith, Harry E. Ramsey
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Abstract : A survey was made of the Lockheed solar patrol films in search of any parameters which could possible be linked with the occurrence of flares. High resolution observations ( or = 1 sec of arc) show that some filaments increase in darkness and become more sharply defined within several hours to several days before the onset of a flare ...
Sara F. Smith, Harry E. Ramsey
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Eruption of a Bifurcated Solar Filament
Solar Physics, 2013We study the partial eruption of a solar filament observed by the Solar Dynamics Observatory (SDO) and the Solar TErrestrial RElations Observatory-Ahead (STEREO-A) spacecraft on 9 May 2012. This filament was located in Active Region NOAA 11475 and consisted of two distinct branches, separated in height above the active region’s primary polarity ...
Chunming Zhu, David Alexander
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Failed Eruptions of Solar Filaments
Astronomy Reports, 2020Solar filaments (prominences), which suddenly and swiftly ascend, i.e., become eruptive, sometimes decelerate and stop at comparatively low altitudes. Causes of failed eruptions generally remain uncertain. The present study analyzes two eruptive phenomena with very similar initial geometries and configurations of external magnetic fields; one of these ...
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Circular Polarization in a Solar Filament
Solar Physics, 2003Integrating 26 624 pairs of video frames, the authors have mapped the circular polarization in an active-region filament against the solar disk by using a traditional magnetograph working at the Hβ line. This filament, offset the disk center, appeared at the boundary of three decayed active regions.
Jingxiu Wang +3 more
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Thin Threads of Solar Filaments
Solar Physics, 2005High-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 +4 more
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Solar Filaments and Photospheric Network
Solar Physics, 2005The 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 +4 more
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The corona associated with solar filaments
Solar Physics, 1981Spectroheliograms 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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