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Problems associated with cool dwarf stars

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Accuracy of Element Abundances from Stellar Atmospheres

Part of the book series: Lecture Notes in Physics ((LNP,volume 356))

Abstract

Models for cool stars differ from those for hotter stars by having complicated state equations and opacities dominated by lines from diatomic and polyatomic molecules. In addition, in cool dwarfs most of the energy transport is by convection, except in the uppermost layers, and methods of handling convection, particularly far away from the adiabatic limit is inadequate. The T(τ) structure of cool dwarfs varies with temperature, gravity and metallicity; therefore scaled solar models cannot be used in analyses. The effective temperature scale of cool dwarfs is also not well known, there being few stars with fundamental temperature measurements.

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Author information

Authors and Affiliations

  1. Mount Stromlo and Siding Spring Observatory, Canberra, Australia

    M. S. Bessell1

  2. Institut für Theoretische Astrophysik, der Universität Heidelberg, Heidelberg, Germany

    M. Scholz

Authors
  1. M. S. Bessell1
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  2. M. Scholz
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Rainer Wehrse

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© 1990 Springer-Verlag

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Bessell1, M.S., Scholz, M. (1990). Problems associated with cool dwarf stars. In: Wehrse, R. (eds) Accuracy of Element Abundances from Stellar Atmospheres. Lecture Notes in Physics, vol 356. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0036066

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  • DOI: https://doi.org/10.1007/BFb0036066

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  • Print ISBN: 978-3-540-52365-9

  • Online ISBN: 978-3-540-46971-1

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