Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity $Z_{\mathrm{ini}}\le 10^{-4}$ in the early Universe I: Effect of surface opacity on the stellar evolution and dust-driven wind

Abstract

Dust formation and resulting mass loss around Asymptotic Giant Branch (AGB) stars with initial metallicity in the range of $0\le Z_{\mathrm{ini}}\le 10^{-4}$ and initial mass $2\le M_{\mathrm{ini}}/M_{\odot }\le 5$ are explored by the hydrodynamical calculations of dust-driven wind (DDW) along the AGB evolutionary tracks. We employ the MESA code to simulate the evolution of stars, assuming an empirical mass-loss rate in the post-main sequence phase, and considering the three types of low-temperature opacities (scaled-solar, CO-enhanced, and CNO-enhanced opacities) to elucidate the effect on the stellar evolution and the DDW. We find that the treatment of low-temperature opacity strongly affects the dust formation and resulting DDW; in the carbon-rich AGB phase, the maximum $\dot{M}$ of $M_{\mathrm{ini}}\ge$ 3 $M_{\odot }$ star with the CO-enhanced opacity is at least one order of magnitude smaller than that with the CNO-enhanced opacity. A wide range of stellar parameters being covered, a necessary condition for driving efficient DDW with $\dot{M}\ge 10^{-6}$ $M_{\odot }$ yr${}^{-1}$ is expressed as the effective temperature $T_{\mathrm{eff}}\lesssim 3850$ K and $\log ({\delta }_{\mathrm{C}}L/{\kappa }_{\mathrm{R}}M)\gtrsim 10.43\log T_{\mathrm{eff}}-32.33$ with the carbon excess ${\delta }_{\mathrm{C}}$ defined as ${\epsilon }_{\mathrm{C}}-{\epsilon }_{\mathrm{O}}$ and the Rosseland mean opacity ${\kappa }_{\mathrm{R}}$ in units of cm${}^2$g${}^{-1}$ in the surface layer, and the stellar mass (luminosity) $M$ $(L)$ in solar units. The derived fitting formulae of gas and dust mass-loss rates in terms of input stellar parameters could be useful for investigating the dust yield from AGB stars in the early Universe being consistent with the stellar evolution calculations.

arXiv comment26 pages, 7 figures, 4 tables, accepted for publication in MNRAS

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