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Transition region quiet sun velocity field evolution
Advances in Space Research, 2002Abstract The UV/EUV SUMER spectrometer aboard SOHO can record profiles of lines emitted by elements at different stages of ionization corresponding to several temperatures within the transition region temperature range. During the solar cycle minimum in July 1996, we were able to observe the quiet Sun during five consecutive days.
Lemaire, P. +5 more
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2019
Total solar eclipses provide a unique view of the faint solar corona, without the bright over-powering emission from the solar disk, enabling us to explore the electron density, temperature, thermodynamics, and related fundamental physics (Habbal et al. 2010a, 2011, 2013).
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Total solar eclipses provide a unique view of the faint solar corona, without the bright over-powering emission from the solar disk, enabling us to explore the electron density, temperature, thermodynamics, and related fundamental physics (Habbal et al. 2010a, 2011, 2013).
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Solar Physics, 1979
Macrospicules have been observed in Hα and He i D3, on the disk and above the limb. In 1975, a rate of 1400 (A⊙day)−1 is inferred, and the ratio of equatorial to polar rates ≲ 2. D3 intensities are a few × 10−3 of the disk center, and do not decrease in coronal holes. The ratio of Hα to D3 intensities is ≈ 10.
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Macrospicules have been observed in Hα and He i D3, on the disk and above the limb. In 1975, a rate of 1400 (A⊙day)−1 is inferred, and the ratio of equatorial to polar rates ≲ 2. D3 intensities are a few × 10−3 of the disk center, and do not decrease in coronal holes. The ratio of Hα to D3 intensities is ≈ 10.
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The Sun's immutable basal quiet atmosphere
Solar Physics, 2003We employ limb darkening, spectral energy distribution (color), and center-disk spectrum line strength to investigate photospheric temporal variability. Current limb-darkening curves agree to 1% with past observations taken at different epochs extending back to 1975.
W. Livingston, L. Wallace
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The fine structure of the quiet Sun
Solar Physics, 1985The observed properties of the small-scale features visible in the quiet photosphere — the granulation, of convective origin, and the network bright points, associated with kG magnetic fields — are described. The known properties of the magnetic flux tubes associated with network bright points are also presented.
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Radio Observations of the Quiet Sun
2004While radio observations of the Sun have mostly focused on active region phenomena, they also contribute unique data to our knowledge of the quiet Sun, in particular through accurate measurements of the temperature as a function of height in the atmosphere and through the measurement of nonthermal emissions from chromospheric and coronal heating events.
Christoph U. Keller, Säam Krucker
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When the Sun Went Strangely Quiet
Science News, 1976The history of science contains more than a few instances in which an old idea or hypothesis, considered improbable, dubious or merely wrong by modern investigators, is, through a combination of new evidence and a more thorough look at the old evidence, shown to be correct after all. Something like this seems to be happening to modern science's view of
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Modelling of Quiet Sun Coronal Structures
International Astronomical Union Colloquium, 1994AbstractThe 1978 paper by Rosner et al. has set the basis for a new way of understanding thermal stratification in the solar corona, taking into account the constraints of magnetic fields on heat conduction. This paper will review recent progress in modelling of coronal loops, and in particular the effects of deviations from Spitzer conductivity ...
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New Scientist, 2010
A compelling link is found between solar activity and harsh winter temperatures in northern ...
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A compelling link is found between solar activity and harsh winter temperatures in northern ...
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