Results 251 to 260 of about 1,066,639 (291)
Helioseismology and solar abundances [PDF]
Physics Reports, 2008 To appear in Physics Reports.
Sarbani Basu, H M Antia
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Solar abundances of oxygen and neon derived from solar wind observations
Astronomy and Astrophysics, 2007 Context.Recently, a revision of the solar abundances of C, N, and O to substantially lower values has led to a controversy on solar opacities in the solar standard model and to the suggestion to revise the solar abundance of neon upward by as much as a ...
P Bochsler
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Space Science Reviews, 1973
Recent spectroscopic results on stellar and solar abundances are reviewed with special reference to (a) Standard abundance distribution (Sun, hot stars, diffuse nebulae); (b) Abundance peculiarities related to stellar evolution (red giants showing results of H-burning and s-process, peculiar and metallic-lined stars); and (c) Population effects that ...
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Recent spectroscopic results on stellar and solar abundances are reviewed with special reference to (a) Standard abundance distribution (Sun, hot stars, diffuse nebulae); (b) Abundance peculiarities related to stellar evolution (red giants showing results of H-burning and s-process, peculiar and metallic-lined stars); and (c) Population effects that ...
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Solar Physics, 1972
Low noise, high resolution spectral scans have been obtained for the resonance lines of silver λ3280.7 and λ3382.9, observed at the centre of the solar disk. A double pass-monochromator is used in conjunction with the Snow telescope at Mount Wilson; the transparency of the sky is monitored during the observations in order to achieve required accuracy ...
John E. Ross, Lawrence H. Aller
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Low noise, high resolution spectral scans have been obtained for the resonance lines of silver λ3280.7 and λ3382.9, observed at the centre of the solar disk. A double pass-monochromator is used in conjunction with the Snow telescope at Mount Wilson; the transparency of the sky is monitored during the observations in order to achieve required accuracy ...
John E. Ross, Lawrence H. Aller
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Nuclear Instruments and Methods, 1970
Abstract There is given a summary of observational and theoretical aspects dealt with in the solar abundance determination. The solar abundance of sixty-six chemical elements are known. The abundance of some of these elements are based on one spectral line only (Ga, Ge, Sn, Er, Yb, Lu, Au, and Th) and the results may be erroneous.
O. Engvold, Ö. Hauge
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Abstract There is given a summary of observational and theoretical aspects dealt with in the solar abundance determination. The solar abundance of sixty-six chemical elements are known. The abundance of some of these elements are based on one spectral line only (Ga, Ge, Sn, Er, Yb, Lu, Au, and Th) and the results may be erroneous.
O. Engvold, Ö. Hauge
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Solar Physics, 1972
From 13 scans obtained with a double-band pass spectrograph at the Snow telescope at Mount Wilson, interpreted by the method of spectral synthesis, the abundance of gold turns out to be log [N(Au)/N(H)] + 12 = 0.70, assuming loggf = − 0.57.
John E. Ross, Lawrence H. Aller
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From 13 scans obtained with a double-band pass spectrograph at the Snow telescope at Mount Wilson, interpreted by the method of spectral synthesis, the abundance of gold turns out to be log [N(Au)/N(H)] + 12 = 0.70, assuming loggf = − 0.57.
John E. Ross, Lawrence H. Aller
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The solar abundance of beryllium
Solar Physics, 1974The solar abundance of beryllium is deduced from high-resolution Kitt Peak observations of the 3130.43- and 3131.08-A lines of Be II interpreted by the method of spectrum synthesis. The results are in good agreement with those previously obtained by Grevesse (1968) and by Hauge and Engvold (1968) and indicate that in the photospheric layers, beryllium
John E. Ross, Lawrence H. Aller
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The solar abundance of germanium
Solar Physics, 1974Spectral scans of the wavelength regions around 3039 A and 3269 A were used as a basis for the determination of the solar abundance of germanium. A solar model similar to the one given by Elste (1968) was used in the analysis of the data. The germanium abundance values obtained are presented in a table.
John E. Ross, Lawrence H. Aller
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Solar Physics, 1972
A preliminary solar Mn abundance of logN(Mn) = 5.41 (logN(H) = 12.00) is derived on the basis of fitting theoretical line profiles which include hyperfine structure (HFS) broadening to the profiles of the λλ 5394.7, 5432.6, and 5537.8 lines of Mn observed at the center of the solar disk with the double-pass spectrograph of the McMath solar telescope at
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A preliminary solar Mn abundance of logN(Mn) = 5.41 (logN(H) = 12.00) is derived on the basis of fitting theoretical line profiles which include hyperfine structure (HFS) broadening to the profiles of the λλ 5394.7, 5432.6, and 5537.8 lines of Mn observed at the center of the solar disk with the double-pass spectrograph of the McMath solar telescope at
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