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16 - Chemical analysis

David F. Gray
David F. Gray
Affiliation:
University of Western Ontario
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Summary

When we look at stellar spectra, we soon recognize the presence of many chemicals. The lines of hydrogen dominate the photospheric spectra of hot stars, but with declining temperature, thousands of lines from other species grow stronger while the lines of hydrogen weaken. One of the tasks of the stellarphotosphere analyst is to disentangle the effects of temperature, pressure, turbulence, and so on from the effects of chemical composition. In broad strokes, the results of chemical analyses tell us that hydrogen is overwhelmingly the most abundant element, comprising ≈90% of the atoms in a normal stellar photosphere, and helium comes next with ≈10%. The remaining elements, often referred to as “metals,” comprise a sprinkling – like salt in a bowl of broth – adding savor and interest. Most of the spectral lines are caused by these low-abundance elements.

Besides our natural curiosity to know what stars are made of, we are motivated to perform chemical composition studies on other fronts. To be more specific, almost any study in stellar atmospheres presupposes some chemical composition. Chemical evidence tells us about the nuclear reactions taking place in stars, internal mixing of material, penetration depths of convection zones, diffusion and gravitational settling, or accretion of material from interstellar space. Lithium and carbon isotope abundances are signatures of the evolutionary stage of a star. The evolution of our galaxy is traceable in part through the differences in chemical composition among stars, since we expect stars formed at different times and in different places to retain information concerning the composition of the material from which they formed.

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The Observation and Analysis of Stellar Photospheres , pp. 384 - 422
Publisher: Cambridge University Press
Print publication year: 2005

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  • Chemical analysis
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.019
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  • Chemical analysis
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.019
Available formats
×

Save book to Google Drive

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

  • Chemical analysis
  • David F. Gray, University of Western Ontario
  • Book: The Observation and Analysis of Stellar Photospheres
  • Online publication: 05 March 2015
  • Chapter DOI: https://doi.org/10.1017/CBO9781316036570.019
Available formats
×