ORIGIN OF THE BIOLOGICALLY IMPORTANT ELEMENTS

@article{Trimble2004ORIGINOT,
  title={ORIGIN OF THE BIOLOGICALLY IMPORTANT ELEMENTS},
  author={Virginia Trimble},
  journal={Origins of life and evolution of the biosphere},
  year={2004},
  volume={27},
  pages={3-21}
}
  • V. Trimble
  • Published 1 December 1997
  • Physics
  • Origins of life and evolution of the biosphere
The chemical elements most widely distributed in terrestrial living creatures are the ones (apart from inert helium and neon) that are commonest in the Universe — hydrogen, oxygen, carbon, and nitrogen. A chemically different Universe would clearly have different biology, if any. We explore here the nuclear processes in stars, the early Universe, and elsewhere that have produced these common elements, and, while we are at it, also encounter the production of lithium, gold, uranium, and other… 

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References

SHOWING 1-10 OF 34 REFERENCES

The origin and abundances of the chemical elements revisited

SummaryThe basic scheme of nucleosynthesis (building of heavy elements from light ones) has held up very well since it was first proposed more than 30 years ago by E.M. Burbidge, G.R. Burbidge,

Chemical Evolution of the Galaxy

Since the discovery of the cosmic microwave background ( 1 84), it is gen­ erally assumed that the universe originated from a hot big bang (78). Detailed nucleosynthesis calculations based on the hot

Abundances of the elements in the solar system

EVOLUTION OF THE STARS AND GAS IN GALAXIES.

Essentially everything of astronomical interest is either part of a galaxy, or from a galaxy, or otherwise relevant to the origin or evolution of galaxies. Diverse examples are that the isotropic

Galacti chemical evolution: Hygrogen through zinc

Using the output from a grid of 60 Type II supernova models (Woosley & Weaver 1995) of varying mass (11 approx. less than (M/solar mass) approx. less than 40) and metallicity (0, 10(exp -4), 0.01,

Synthesis of the Elements in Stars

Man inhabits a universe composed of a great variety of elements and their isotopes. In Table I,1 a count of the stable and radioactive elements and isotopes is listed. Ninety elements are found

Energy Production in Stars

Abstract Recent work and trends in the field of stellar energy production and related topics are reviewed. Thermonuclear reactions are discussed in general, and a list is given of those reactions

The Origin and Abundance Distribution of the Elements

astrophysics suggests that our present universe has a definite age, that the observed rela­ tive abund ances appear to be universal quant ities, and that the physical conditions required for nuclear

Thep-nuclei: abundances and origins

SummaryThe review discusses the solar system (meteoritic) abundances and the possible modes of nucleosynthesis of the 30-oddp-nuclei from74Se to196Hg. In addition to a discussion of the abundances