dc.contributor.author | Vincenzo, Fiorenzo | |
dc.contributor.author | Kobayashi, Chiaki | |
dc.date.accessioned | 2020-07-28T00:06:27Z | |
dc.date.available | 2020-07-28T00:06:27Z | |
dc.date.issued | 2020-07-01 | |
dc.identifier.citation | Vincenzo , F & Kobayashi , C 2020 , ' Stellar migrations and metal flows -- Chemical evolution of the thin disc of a simulated Milky Way analogous galaxy ' , Monthly Notices of the Royal Astronomical Society , vol. 496 , no. 1 , staa1451 , pp. 80–94 . https://doi.org/10.1093/mnras/staa1451 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/2004.08050v1 | |
dc.identifier.other | ORCID: /0000-0002-4343-0487/work/78165673 | |
dc.identifier.uri | http://hdl.handle.net/2299/23008 | |
dc.description | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 496, Issue 1, July 2020, Pages 80–94 ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. | |
dc.description.abstract | In order to understand the roles of metal flows in galaxy formation and evolution, we analyse our self-consistent cosmological chemo-dynamical simulation of a Milky Way like galaxy during its thin-disc phase. Our simulated galaxy disc qualitatively reproduces the variation of the dichotomy in [$\alpha$/Fe]-[Fe/H] at different Galactocentric distances as derived by APOGEE-DR16, as well as the stellar age distribution in [$\alpha$/Fe]-[Fe/H] from APOKASC-2. The disc grows from the inside out, with a radial gradient in the star-formation rate during the entire phase. Despite the radial dependence, the outflow-to-infall ratio of metals in our simulated halo shows a universal (time-independent) profile scaling with the disc growth. The simulated disc undergoes two modes of gas inflow: (i) an infall of metal-poor and relatively low-[$\alpha$/Fe] gas, and (ii) a radial flow where already chemically-enriched gas moves inwards with an average velocity of $\sim0.7$ km/s. Moreover, we find that stellar migrations mostly happen outwards, on typical time scales of $\sim5$ Gyr. Our predicted radial metallicity gradients agree with the observations from APOGEE-DR16, and the main effect of stellar migrations is to flatten the radial metallicity profiles by 0.05 dex/kpc in the slopes. We also show that the effect of migrations can appear more important in [$\alpha$/Fe] than in the [Fe/H]-age relation of thin-disc stars. | en |
dc.format.extent | 15 | |
dc.format.extent | 8051498 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | astro-ph.GA | |
dc.title | Stellar migrations and metal flows -- Chemical evolution of the thin disc of a simulated Milky Way analogous galaxy | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.description.status | Peer reviewed | |
dc.identifier.url | https://arxiv.org/abs/2004.08050 | |
rioxxterms.versionofrecord | 10.1093/mnras/staa1451 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |