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The [α/Fe] versus [Fe/H] diagram refers to the graph, commonly used in stellar and galactic astrophysics, which shows the logarithmic ratio number densities of diagnostic elements compared to the solar value. The x-axis shows the abundance of elements iron (Fe) vs. hydrogen (H), that is, [Fe/H]. The y-axis shows the combination of one or several of the alpha process elements (O, Ne, Mg, Si, S, Ar, Ca, and Ti) compared to iron (Fe), that is, [α/Fe].

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  • (α/Fe) versus (Fe/H) diagram (en)
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  • The [α/Fe] versus [Fe/H] diagram refers to the graph, commonly used in stellar and galactic astrophysics, which shows the logarithmic ratio number densities of diagnostic elements compared to the solar value. The x-axis shows the abundance of elements iron (Fe) vs. hydrogen (H), that is, [Fe/H]. The y-axis shows the combination of one or several of the alpha process elements (O, Ne, Mg, Si, S, Ar, Ca, and Ti) compared to iron (Fe), that is, [α/Fe]. (en)
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  • The [α/Fe] versus [Fe/H] diagram refers to the graph, commonly used in stellar and galactic astrophysics, which shows the logarithmic ratio number densities of diagnostic elements compared to the solar value. The x-axis shows the abundance of elements iron (Fe) vs. hydrogen (H), that is, [Fe/H]. The y-axis shows the combination of one or several of the alpha process elements (O, Ne, Mg, Si, S, Ar, Ca, and Ti) compared to iron (Fe), that is, [α/Fe]. These diagrams allow one to assess the nucleosynthesis channels and Galactic evolution of samples of stars to first order and are one of the most commonly used tools of Galactic population analysis of our Milky Way. The diagrams are using abundance ratios that are normalised to the Sun (placing the Sun at (0,0) in the diagram) and allow to easily identify stars of the Galactic stellar high-alpha disk (historically known as the Galactic stellar thick disk) via their typically enhanced in [α/Fe] and stars of the Galactic stellar low-alpha disk (historically known as the Galactic stellar thin disk) having [α/Fe] as low as the Sun. It further allows to identify stars that are likely born at times or in environments very different to the stellar disk, typically metal-poor stars (with low [Fe/H] < -1) which likely belong to the stellar halo or accreted features. (en)
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