Results 291 to 300 of about 1,350,678 (342)

Small-amplitude oscillations in solar filaments

Astronomy Reports, 2012
The temporal and spatial properties of small-amplitude oscillations have been studied using spectral observations of motions in solar filaments carried out at the Sayan Solar Observatory (Institute of Solar-Terrestrial Physics, Russian Academy of Sciences).
G. P. Mashnich, V. S. Bashkirtsev, A. I. Khlystova   +2 more
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Large-scale motion of solar filaments

Journal of Astrophysics and Astronomy, 2000
AbstractPrecise 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
openaire   +1 more source

Activity cycle of solar filaments

Journal of Astrophysics and Astronomy, 2007
Long-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, Q. X. Li, P. X. Gao, J. Mu, H. D. Chen, T. W. Su   +5 more
openaire   +1 more source

Periodic Motion Along Solar Filaments

Solar Physics, 2006
We present observations of four filaments that exhibit large-amplitude periodic mass motion. Observations are obtained using the high resolution (2″) and high cadence (1 min) Hα telescope system at the Big Bear Solar Observatory (BBSO). The motions found in these events are along the axis of the filaments, and are associated with the activity of a ...
Ju Jing, Jeongwoo Lee, Thomas J. Spirock, Haimin Wang   +3 more
openaire   +1 more source

SOLAR FILAMENT STRUCTURE

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
openaire   +1 more source

Activated solar filaments and flares

Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences, 1980
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. Therefore, until very recently, filament disruptions were considered as interesting, but physically insignificant, flare ...
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Circular Polarization in a Solar Filament

Solar Physics, 2003
Integrating 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, Guiping Zhou, Yuming Wang, Limin Song   +3 more
openaire   +1 more source

Differential Rotation of Solar Filaments Early Observed by the OGAUC in the Period 1929 – 1941

Solar Physics, 2022
M. Wan, Ke-Jun Li
semanticscholar   +1 more source

Disappearing solar filaments and geomagnetic activity

Nature, 1982
Early attempts to link solar filaments and their disappearances with geomagnetic activity1–7 were inconclusive. Joselyn and McIntosh8 have suggested that some magnetic storms are produced by disappearing filaments. However, we feel that their study included too few cases to establish this link conclusively because, of the 12 possible filament–storm ...
L. F. McNamara, C. S. Wright
openaire   +1 more source

Solar filaments as tracers of subsurface processes

Journal of Astrophysics and Astronomy, 2000
AbstractSolar filaments are discussed in terms of two contrasting paradigms. The standard paradigm is that filaments are formed by condensation of coronal plasma into magnetic fields that are twisted or dimpled as a consequence of motions of the fields’ sources in the photosphere.
openaire   +1 more source