Results 181 to 190 of about 961,519 (212)

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 potassium abundance in the solar photosphere

Solar Physics, 1975
High precision center-limb spectrograms of the K i resonance doublet line at λ 7699 A were used to study the line formation and to determine the abundance of potassium in the solar atmosphere. The LTE assumption is not valid for these lines. Synthetic profiles computed in NLTE reproduce very well the observed center-limb line behaviour and yield logɛ
Ramiro De La Reza, Edith A. Müller
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Temperature variations in the solar photosphere

Solar Physics, 1974
From the variations in equivalent width of a selected set of Fraunhofer lines, we derived the variation of effective temperature and microturbulence velocity between the equator and the regions at heliographic latitude of ∼- 72°. The reliability of the results (ΔT/T = 0 ± 0.6%, Δξ/ξ = 6% ± 13%) needs further investigations, but from the analysis of our
R. Falciani, M. Rigutti, G. Roberti
openaire   +1 more source

The solar photospheric abundance of iron

Solar Physics, 1975
A new value of the solar photospheric abundance of iron, independent of line-shape parameters, is derived.
E. Bi�mont, N. Grevesse
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Temperature variations in the solar photosphere

Solar Physics, 1973
Detailed LTE calculations were made of the sensitivities of some Fraunhofer lines to local variations of the effective temperature of the Sun, taking also into account the effects of local variations of the microturbulence. The temperature sensitivities show a clear dependence upon the mean optical depth at which lines originate and upon the binding ...
B. Caccin, A. Donati-Falchi, R. Falciani
openaire   +1 more source

The Location of Solar Oscillations in the Photosphere

2001
Applying a correlation analysis to time series of granulation it has been shown that due to the influence of enhanced turbulent motions near the downflow regions in the intergranular lanes the turbulent motions predominate.
A. Hanslmeier, A. Kučera, J. Rybák, H. Wöhl   +3 more
openaire   +1 more source

Temperature fluctuations in the solar photosphere

Solar Physics, 1969
The general problem of interpreting granulation data, in particular Edmonds' r.m.s. intensity fluctuation distribution against heliocentric angle θ, is discussed.
openaire   +1 more source

4.1.1.4 Solar photosphere and chromosphere

2009
Traditionally, the atmosphere of the Sun has been divided into four layers, starting with the photosphere at the bottom, followed by the chromosphere, the transition region, and the corona as the outermost region. The photosphere is a layer of only a few hundred kilometers thickness in which the temperature drops outwards from around 6000 K at the ...
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The universality of power law slopes in the solar photosphere and transition region observed with HMI and IRIS

Frontiers in Astronomy and Space Sciences, 2023
Markus Aschwanden
exaly  

Granules of the Solar Photosphere

Scientific American, 1936
openaire   +1 more source