Observations and Theories of Mixing in Red Giants

Scalo, John M.

doi:10.1007/978-94-009-8492-9_9

Observations and Theories of Mixing in Red Giants

John M. Scalo³

Conference paper

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11 Citations

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 88))

Abstract

Available data on abundances, luminosities, masses, technetium line strengths, and other properties of the peculiar red giants of the disk population are reviewed in order to provide a set of observational constraints on proposed theories of mixing and nucleosynthesis during advanced red giant evolution. The observations suggest that mixing occurs in stars of all masses, ages, and compositions, sets in by a core mass of about 0.5 M_⊙ in double-shell models, and either terminates by a core mass of about 0.8 M_⊙ or is stochastic in nature, with different mixing probabilities for stars of the same initial mass and composition. Evidence concerning luminosities, s-process abundance distributions, and Mg and Ti isotopic ratios in these stars imply that ²²Ne(α,n)²⁵Mg is not the neutron source in most observed peculiar red giants, which have small masses. None of the constraints are satisfied by existing stellar evolution calculations. A number of potentially important physical effects which may lead to mixing, involving turbulence phenomena, magnetic fields, and rotational instabilities, are reviewed.

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Department of Astronomy, University of Texas at Austin, Austin, Texas, 78712, USA
John M. Scalo

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Department of Astronomy, University of Illinois at Urbana-Champaign, USA
Icko Iben Jr.
Osservatorio Astronomico, Universitè di Bologna, Italy
Alvio Renzini

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Scalo, J.M. (1981). Observations and Theories of Mixing in Red Giants. In: Iben, I., Renzini, A. (eds) Physical Processes in Red Giants. Astrophysics and Space Science Library, vol 88. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8492-9_9

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