Results 261 to 270 of about 1,066,639 (291)
Some of the next articles are maybe not open access.
SOLAR ABUNDANCES OF THE ELEMENTS
Meteoritics, 1983The isotopic compositions of noble gases in the solar wind show high enrichments of light isotopes. When corrected for mass fractionation all five noble gases there can be resolved in terms of the two primitive noble gas components that have been identified in planetary solids.
O.K. Manuel, Golden Hwaung
openaire +1 more source
The solar abundance of tungsten
Solar Physics, 1982Recent measurements of Wi oscillator strengths (Obbarius and Kock, 1982) lead to a solar photospheric abundance of tungsten, log ɛW = 1.06 ± 0.15 on the scale log ɛH = 12. The solar W/Si abundance ratio, 0.32 W atoms/106 Si, coincides with that found in carbonaceous chrondrites. Implications for solar-system r-processes abundances are pointed out.
Hartmut Holweger, Klaus Werner
openaire +1 more source
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
openaire +1 more source
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
openaire +1 more source
Abundances in the solar corona
Advances in Space Research, 1997Abstract A large number of papers over the past 15 years have commented on solar coronal abundances and how they differ from photospheric values. The simple pattern of enhancement or depletion with element first ionization potential (FIP) has been called into question by recent data, however.
openaire +1 more source
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
openaire +1 more source
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
openaire +1 more source
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
openaire +1 more source
The solar abundance of titanium
Solar Physics, 1976A solar titanium abundance has been derived from measurements of eight selected very weak lines.
openaire +1 more source
Solar Neutrinos and the Solar Helium Abundance *
Physical Review Letters, 1968openaire +1 more source