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- W2965604673 abstract "We investigate how the stellar and gas-phase He abundances evolve as a function of time within simulated star-forming disc galaxies with different star formation histories. We make use of a cosmological chemodynamical simulation for galaxy formation and evolution, which includes star formation as well as energy and chemical enrichment feedback from asymptotic giant branch stars, core-collapse supernovae, and Type Ia supernovae. The predicted relations between the He mass fraction, Y , and the metallicity, Z , in the interstellar medium of our simulated disc galaxies depend on the galaxy star formation history. In particular, dY /dZ is not constant and evolves as a function of time, depending on the specific chemical element that we choose to trace Z ; in particular, dY /dX O and dY /dX C increase as a function of time, whereas dY /dX N decreases. In the gas-phase, we find negative radial gradients of Y , due to the inside-out growth of our simulated galaxy discs as a function of time; this gives rise to longer chemical enrichment timescales in the outer galaxy regions, where we find lower average values for Y and Z . Finally, by means of chemical-evolution models, in the galactic bulge and inner disc, we predict steeper Y vs. age relations at high Z than in the outer galaxy regions. We conclude that for calibrating the assumed Y − Z relation in stellar models, C, N, and C+N are better proxies for the metallicity than O because they show steeper and less scattered relations." @default.
- W2965604673 created "2019-08-13" @default.
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- W2965604673 date "2019-10-01" @default.
- W2965604673 modified "2023-09-26" @default.
- W2965604673 title "He abundances in disc galaxies - I. Predictions from cosmological chemodynamical simulations" @default.
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