Results 11 to 20 of about 1,066,639 (291)
Measuring Solar Abundances [PDF]
AIP Conference Proceedings, 2001 © 2001 American Institute of Physics. Issue Date: 21 November 2001. We gratefully acknowledge the effort of the scientific and local organisation committees, in particular of Robert F. Wimmer-Schweingruber, in making this workshop happen. We also thank Sylvie Vauclair and Robert F. Wimmer-Schweingruber for useful comments on the manuscript.
von Steiger, R. +17 more
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Solar abundance of osmium [PDF]
Proceedings of the National Academy of Sciences, 1976 The abundance parameter, log gfA , where g is the statistical weight of the lower level, f is the oscillator strength, and A is the abundance (by numbers of atoms with ...
G, Jacoby, L H, Aller
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Solar abundance of platinum [PDF]
Proceedings of the National Academy of Sciences, 1975 Three lines of neutral platinum, located at λ 2997.98 Å, λ 3064.71 Å, and λ 3301.86 Å have been used to determine the solar platinum abundance by the method of spectral synthesis. On the scale, log A (H) = 12.00, the thus-derived solar platinum abundance is 1.75 ± 0.10, in fair accord with ...
H, Burger, L H, Aller
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Solar Abundance of Gallium [PDF]
Proceedings of the National Academy of Sciences, 1970 The spectral region around the λ4172 Å resonance line of gallium has been synthesized at disk positions μ = 1.0, 0.5, and 0.3. The center-limb variation can be reproduced by Elste's semiempirical model if a macroturbulent smearing of the emergent spectrum due to mass motions with mean velocity decreasing with altitude are introduced.
J, Ross, L, Aller
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Solar abundance of iridium [PDF]
Proceedings of the National Academy of Sciences, 1976 By a method of spectrum synthesis, which yields log gfA , where g is the statistical weight of the lower level, f is the oscillator strength, and A is the abundance, an ...
S, Drake, L H, Aller
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THE SOLAR FLARE IRON ABUNDANCE [PDF]
The Astrophysical Journal, 2012 The abundance of iron is measured from emission line complexes at 6.65 keV (Fe line) and 8 keV (Fe/Ni line) in {\em RHESSI} X-ray spectra during solar flares. Spectra during long-duration flares with steady declines were selected, with an isothermal assumption and improved data analysis methods over previous work.
Phillips, K. J. H., Dennis, B. R.
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SOLAR MODELS WITH REVISED ABUNDANCE [PDF]
The Astrophysical Journal, 2011 We present new solar models in which we use the latest low abundances and we further include the effects of rotation, magnetic fields and extra-mixing processes. We assume that the extra-element mixing can be treated as a diffusion process, with the diffusion coefficient depending mainly on the solar internal configuration of rotation and magnetic ...
Bi, Shaolan +3 more
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Elemental Abundances Of Solar Sibling Candidates [PDF]
, 2014 Dynamical information along with survey data on metallicity and in some cases age have been used recently by some authors to search for candidates of stars that were born in the cluster where the Sun formed.
Ramirez, Ivan +15 more
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THE LTE SOLAR ABUNDANCE OF NEODYMIUM [PDF]
Al-Azhar Bulletin of Science, 2014 We study the solar photospheric abundance of singly ionized neodymium (Nd II) using high resolution spectroscopic data obtained by Fourier transform spectrograph (FTS). Based on the Local Thermodynamical Equilibrium (LTE) assumption, a new value of Nd abundance is derived.
Abdelkawy, A. G. A. +3 more
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