The Chemical Composition of the Sun and the Solar System

@article{Aller1968TheCC,
  title={The Chemical Composition of the Sun and the Solar System},
  author={Lawrence Hugh Aller},
  journal={Publications of the Astronomical Society of Australia},
  year={1968},
  volume={1},
  pages={133 - 135}
}
  • L. Aller
  • Published 1 December 1968
  • Physics, Geology
  • Publications of the Astronomical Society of Australia
A knowledge of the quantitative chemical composition of the primordial solar system must underlie all comprehensive studies of its origin and evolution. Usually we take the composition of the surface layers (photosphere) of the Sun as representative of this composition (except perhaps for deuterium, Li, B, and Be). 
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References

SHOWING 1-10 OF 24 REFERENCES

Abundance of Helium in the Sun

THE observed abundances of elements are largely understood in terms of stellar nucleosynthesis. The origin of helium, however, remains a major problem. Indeed, Hoyle and Tayler1 concluded that the

THE ABUNDANCES OF THE ELEMENTS IN THE SOLAR PHOTOSPHERE-VI

Summary Low noise photoeleetrie seans of the Rb I resonanee lines (A,\ 7800 and 7947) have been obtained with the Oxford spectrometer. An analysis results in an improved abundanee determination. log

The abundance of lead in the sun.

The nuclear stability of lead and its role as the end product of decay schemes of naturally occurring radioactive elements lend this metal a peculiar importance in geochronology and cosmology. A

OSCILLATOR STRENGTHS OF LEAD AND THE LEAD ABUNDANCE IN THE SUN

The oscillator strengths of four transitions in neutral lead were calculated and compared with recent experimental results. The method of calculation is described. These values are used to

Center-to-limb analysis of the solar oxygen lines

Several lines of neutral oxygen observed at various positions on the solar disk were used to study the influence of (1) the temperature distribution, (2) the velocity field, and (3) the damping on

Yttrium abundance in the sun.

Solar abundance of Y derived from Y II lines by computing transition probabilities and oscillator strength involving several configurations