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Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity $Z_{ini} <= 10^{-4}$ in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind
| Title: | Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity $Z_{ini} <= 10^{-4}$ in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind |
| Authors: | Tashibu, Shohei Browse this author | | Yasuda, Yuki Browse this author | | Kozasa, Takashi Browse this author →KAKEN DB |
| Keywords: | stars: abundances | | stars: AGB and post-AGB | | ISM: abundances | | dust, extinction |
| Issue Date: | Apr-2017 |
| Publisher: | Oxford University Press |
| Journal Title: | Monthly notices of the royal astronomical society |
| Volume: | 466 |
| Issue: | 2 |
| Start Page: | 1709 |
| End Page: | 1732 |
| Publisher DOI: | 10.1093/mnras/stw3160 |
| Abstract: | Dust formation and the resulting mass loss around asymptotic giant branch (AGB) stars with initial metallicity in the range $0 ≤ Z_{ini} ≤ 10^{-4}$ and initial mass $2 ≤ M_{ini}/M_⦿ ≤ 5$ are explored by hydrodynamical calculations of the 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 three types of low-temperature opacity (scaled-solar, CO-enhanced and CNO-enhanced opacity) to elucidate the effect on stellar evolution and the DDW. We find that the treatment of low-temperature opacity strongly affects dust formation and the resulting DDW; in the carbon-rich AGB phase, the maximum. $\dot{M}$ of $M_{ini} ≥ 3M_⦿$ stars 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, the necessary condition for driving efficient DDW with. $\dot{M} ≥ 10^{-6} M_⦿ yr^{-1}$ is expressed as effective temperature $T_{eff} ≲ 3850 K$ and $\log(\delta_CL/\kappa_RM) ≳ 10.43 \log T_{eff} -32.33$, with the carbon excess $\delta_C$ defined as $\epsilon_C - \epsilon_O$, the Rosseland mean opacity. $\kappa_R$ in units of $cm^2 g^{-1}$ in the surface layer and the stellar mass (luminosity) $M(L)$ in solar units. The fitting formulae derived for 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 stellar evolution calculations. |
| Rights: | This article has been accepted for publication in Monthly notices of the royal astronomical society ©2016 The Authors Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved. |
| Type: | article |
| URI: | http://hdl.handle.net/2115/66490 |
| Appears in Collections: | 理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)
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Submitter: 小笹 隆司
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