Atomic diffusion during red giant evolution

Details Atomic diffusion during red giant evolution Atomic diffusion during red giant evolution

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...510a.104m&link_type=abstract

Astronomy and Astrophysics, Volume 510, id.A104

Astronomy and Astrophysics

Astrophysics

9

Diffusion, Stars: Evolution, Stars: Population Ii, Stars: Interiors, Stars: Abundances

Scientific paper

Atomic diffusion has been found to play a role during most stellar evolution stages. Its effect is studied during the relatively rapid red giant (RG) phase to determine the concentration variations it leads to and at what accuracy level it can be safely neglected. A model calculated with atomic diffusion to the helium flash is compared to one calculated without any atomic diffusion and to one calculated with atomic diffusion up to a point on the subgiant branch well past the turnoff but without diffusion thereafter. For stars with a metallicity of Z=10-4, it was found that the mass of the helium core at which the He flash occurs is 0.0026 M&sun; larger in the presence of atomic diffusion. The difference decreases to 0.0017 M&sun; as metallicity is increased to Z = 0.02. Radiative accelerations are found to play an interesting role around the hydrogen burning shell. The atomic diffusion of 4He is also shown to lead to a larger μ inversion than 3He burning. Its potential role in mixing between the burning shell and the surface convection zone is investigated. Whether one may neglect atomic diffusion during the RG phase depends on the required accuracy. It is not so negligible as one may have expected but still only reduces by about 0.02 dex the luminosity of the RG branch bump. The way it modifies the mass of the core when the flash occurs depends on metallicity.

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