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Chemical Environment and Temperature Effects on the Formation and Destruction of C<sub>3</sub>O<sub>2</sub> in Cosmic-Ray-Processed Ices. [PDF]
ACS OmegaPilling S +3 more
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Evidence that freshwater mussels attempt temporal partitioning of their host fishes. [PDF]
Sci RepSmodis SL, Morris TJ, Ackerman JD.
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Carbon monoxide dehydrogenase-encoding microorganisms in volcanic astrobiological analogues: an enzyme system to investigate the evolution of life. [PDF]
FEMS Microbiol EcolLatorre V +3 more
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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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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, 1975
The solar Nb abundance is derived from five Nb i and ten Nb ii lines in the photospheric spectrum. Equivalent widths are obtained from measurements on spectra recorded at Kitt Peak National Observatory. Synthetic spectrum calculations gave abundances of 2.23 and 2.08 from neutral and ionized lines respectively in the logarithmic AH = 12.00 scale.
�. Hauge, Naked H. Youssef
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The solar Nb abundance is derived from five Nb i and ten Nb ii lines in the photospheric spectrum. Equivalent widths are obtained from measurements on spectra recorded at Kitt Peak National Observatory. Synthetic spectrum calculations gave abundances of 2.23 and 2.08 from neutral and ionized lines respectively in the logarithmic AH = 12.00 scale.
�. Hauge, Naked H. Youssef
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Solar abundance of praseodymium
Solar Physics, 197916 lines of Pr ii possibly present in the solar photospheric spectrum have been studied. When including hyperfine structure in synthetic calculations, investigations of 9 lines result in an abundance APr = 0.71 ± 0.08 in the log AH = 12.00 scale.
Emile Bi�mont +2 more
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Solar Physics, 1976
The solar Hf abundance is determined using nine Hf ii lines in the photospheric spectrum. The transition probabilities were obtained from lifetime measurements performed by the beam-foil technique. The abundance derived from synthetic spectrum calculations is A(Hf) = 0.88 ± 0.08 in the logarithmic A(H) = 12.00 scale.
T. Andersen, P. Petersen, �. Hauge
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The solar Hf abundance is determined using nine Hf ii lines in the photospheric spectrum. The transition probabilities were obtained from lifetime measurements performed by the beam-foil technique. The abundance derived from synthetic spectrum calculations is A(Hf) = 0.88 ± 0.08 in the logarithmic A(H) = 12.00 scale.
T. Andersen, P. Petersen, �. Hauge
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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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