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Dust formation and resulting mass loss around Asymptotic Giant Branch (AGB)stars with initial metallicity in the range of $0 \leq Z_{\rm ini} \leq10^{-4}$ and initial mass $2\leq M_{\rm ini}/M_{\odot} \leq 5$ are explored bythe hydrodynamical calculations of dust-driven wind (DDW) along the AGBevolutionary tracks. We employ the MESA code to simulate the evolution ofstars, 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 stellarevolution and the DDW. We find that the treatment of low-temperature opacitystrongly affects the dust formation and resulting DDW; in the carbon-rich AGBphase, the maximum $\dot{M}$ of $M_{\rm ini} \geq$ 3 $M_{\odot}$ star with theCO-enhanced opacity is at least one order of magnitude smaller than that withthe CNO-enhanced opacity. A wide range of stellar parameters being covered, anecessary condition for driving efficient DDW with $\dot{M} \ge 10^{-6}$$M_{\odot}$ yr$^{-1}$ is expressed as the effective temperature $T_{\rm eff}\lesssim 3850$ K and $\log(\delta_{\rm C}L/\kappa_{\rm R} M) \gtrsim 10.43\logT_{\rm eff}-32.33 $ with the carbon excess $\delta_{\rm C}$ defined as$\epsilon_{\rm C} - \epsilon_{\rm O}$ and the Rosseland mean opacity$\kappa_{\rm R}$ in units of cm$^2$g$^{-1}$ in the surface layer, and thestellar mass (luminosity) $M$ $(L)$ in solar units. The derived fittingformulae of gas and dust mass-loss rates in terms of input stellar parameterscould be useful for investigating the dust yield from AGB stars in the earlyUniverse being consistent with the stellar evolution calculations.

monthly notices of the royal astronomical society

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