Volume 529, May 2011
|Number of page(s)||20|
|Section||Stellar structure and evolution|
|Published online||01 April 2011|
Black-and-white version of Fig. 4. Gray-coded concentrations in two HB stars of the same metallicity after 25 Myr on the HB. Left panel with a Teff of 14 000 K (0.59 M⊙) and right panel of 30 100 K (0.51 M⊙). The scale of the radius is linear, but the logarithmic value of the mass coordinate above a number of points, log ΔM/M∗, is shown to the left of the horizontal black line. The concentration scale is given in the right insert. Small circles near the top of the left panel mark the extent of the surface convection zone, while similar circles near the center of both models mark the central convection zone. The small inset in between the two panels shows the high Teff star on the radius scale of the low Teff star. For −7 < log ΔM/M∗ < −4 the concentration is quite different for many species. It is surprisingly so for C and O for log ΔM/M∗ > −2.
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Some of the properties of all evolutionary models calculated, grouped by metallicity. All models in Figs. B.1 to B.4 were calculated with a turbulent diffusion coefficient given by Eqs. (1) and (3) with ΔM0 = 10-7.5 M⊙. See Sect. 2.
Models with Z0 = 0.0001. The curves are identified in the figure by the mass of the HB model. The color code is the same as used for the left panel of Fig. 2 and is defined in footnote . Zero age HB is defined as the moment when X(12C) reaches 0.04. In the figures the curves are not all very precisely aligned to that value. X0(surfFe) identifies the Fe mass fraction in the original main-sequence model, similarly for the other species.
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Models illustrated in this article, with their ZAHB characteristics.
© ESO, 2011
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