Results 171 to 180 of about 41,536 (207)

Comprehensive studies of solar activity on the CORONAS-F satellite

Astronomy Letters, 2002
The first results of comprehensive CORONAS-F observations of solar activity are presented. The CORONAS-F instrumentation and principal scientific objectives are briefly described and examples of the first results of data reduction are given.
V. N. Oraevsky, I. I. Sobelman
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Prominences and the Green Corona Over the Solar Activity Cycle

Solar Physics, 1998
Prominences, in contrast to other solar activity features, may appear at all heliographic latitudes. The position of zones where prominences are mainly concentrated depends on the cycle phase of solar activity. It is shown, for prominence observations made at Lomnický Stit over the period 1967–1996, how the position of prominence zones changes over a ...
M. Minarovjech, M. Rybanský, V. Rušin
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Development of a complex of activity in the solar corona

Solar Physics, 1977
Skylab observations of the Sun in soft X-rays gave us the first possibility to study the development of a complex of activity in the solar corona during its whole lifetime of seven solar rotations. The basic components of the activity complex were permanently interconnected (including across the equator) through sets of magnetic field lines, which ...
Robert Howard, Zdeněk Švestka
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Quiet corona density model for the last maximum of solar activity

Solar Physics, 1973
We have selected observations of quiet K corona in maximum activity phase (1970 and 1972) and we have computed the corresponding density models. The density is found to be two times smaller than in average maximum coronal models (Newkirk, 1967) and nearly equal to that of minimum coronas (Saito, 1970).
Y. Leblanc, J. L. Leroy, P. Pecantet
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STRUCTURE AND DYNAMICS OF THE SOLAR CORONA DURING DIFFERENT PHASES OF SOLAR ACTIVITY

БЛИЗКИЯТ КОСМОС – ОБЩА ЦЕЛ
The structure, shape and brightness of the solar corona significantly depend on the activity of the Sun. The crown is very bright and even at maximum solar activity. On these same composite photographs we can observe very bright coronal streamers and other active areas.
Stoeva, P., Stoev, A., Kostov, M.
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Results of Spectral Corona Observations in Solar Activity Cycles 17–24

Geomagnetism and Aeronomy, 2017
The results of the work of the global observation network are considered, and a comparative analysis of the data of various coronal observatories is performed. The coronal activity index has been reconstructed for the period 1939–2016 based on the data of various observatories in Kislovodsk system. For this purpose, the corona daily intensity maps from
A. Kh. Aliev, S. A. Guseva, A. G. Tlatov
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Variations in solar shortwave radiation in the solar activity cycle as measured by the CORONAS satellites

Solar System Research, 2008
The CORONAS-I and CORONAS-F data on variations in the ionizing shortwave ultraviolet (UV) solar radiation (EUV radiation) at wavelengths of less than 130 nm and near the H Lyman-alpha line are presented. The CORONAS-I data refer to the period close to solar minimum (the index F 10.7 = 80−100), and the CORONAS-F measurements were
T. V. Kazachevskaya, A. A. Nusinov, V. V. Katyushina, D. A. Gonjyukh   +3 more
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Confined pseudo-shocks as an energy source for the active solar corona

Nature Astronomy, 2018
The Sun’s active corona requires an energy flux of ~103 W m−2 to compensate for radiative losses and to maintain its high temperature1. Plasma moves in the corona through magnetic loops2,3, which may be connected with the flows in and around sunspots4–6.
Abhishek Kumar Srivastava, Krzysztof Murawski, Blażej Kuźma, Dariusz Patryk Wójcik, Teimuraz V. Zaqarashvili, Marco Stangalini, Zdzislaw E. Musielak, John Gerard Doyle, Pradeep Kayshap, Bhola N. Dwivedi   +9 more
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The outer solar corona during the declining portion of the solar activity cycle

Planetary and Space Science, 1966
Abstract Some hitherto unpublished observations of the coronal radio scattering made in Sydney during 1962 are combined with observations made at various observatories in the two year interval 1960–1962 to deduce the dependence of scattering on solar activity in the range of angular separations 20–80 R⊙.
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New Method of Forecasting Geomagnetic Activity using Features of the Solar Corona

Nature, 1968
EARLIER studies1,2 have shown that a geomagnetic disturbance will occur when, and only when, a coronal formation is directed towards the Earth. An idea of the features and the temporal changes of the solar corona which are not currently observable can be acquired through the known relations between coronal formations and prominences.
B. BEDNÁŘOVÁ-NOVÁKOVÁ, J. HALENKA
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