Skip to main content

Research Repository

Advanced Search

The chemical evolution of the solar neighbourhood for planet-hosting stars

Pignatari, Marco; Trueman, Thomas C.L.; Womack, Kate A.; Gibson, Brad K.; Côte, Benoit; Turrini, Diego; Sneden, Christopher; Mojzsis, Stephen J.; Stancliffe, Richard J.; Fong, Paul; Lawson, Thomas V.; Keegans, James D.; Pilkington, Kate; Passy, Jean Claude; Beers, Timothy C.; Lugaro, Maria

Authors

Marco Pignatari

Thomas C.L. Trueman

Kate A. Womack

Brad K. Gibson

Benoit Côte

Diego Turrini

Christopher Sneden

Stephen J. Mojzsis

Richard J. Stancliffe

Paul Fong

James D. Keegans

Kate Pilkington

Jean Claude Passy

Timothy C. Beers

Maria Lugaro



Abstract

Theoretical physical-chemical models for the formation of planetary systems depend on data quality for the Sun's composition, that of stars in the solar neighbourhood, and of the estimated 'pristine' compositions for stellar systems. The effective scatter and the observational uncertainties of elements within a few hundred parsecs from the Sun, even for the most abundant metals like carbon, oxygen and silicon, are still controversial. Here we analyse the stellar production and the chemical evolution of key elements that underpin the formation of rocky (C, O, Mg, Si) and gas/ice giant planets (C, N, O, S). We calculate 198 galactic chemical evolution (GCE) models of the solar neighbourhood to analyse the impact of different sets of stellar yields, of the upper mass limit for massive stars contributing to GCE (Mup) and of supernovae from massive-star progenitors which do not eject the bulk of the iron-peak elements (faint supernovae). Even considering the GCE variation produced via different sets of stellar yields, the observed dispersion of elements reported for stars in the Milky Way (MW) disc is not reproduced. Among others, the observed range of super-solar [Mg/Si] ratios, sub-solar [S/N], and the dispersion of up to 0.5 dex for [S/Si] challenge our models. The impact of varying Mup depends on the adopted supernova yields. Thus, observations do not provide a constraint on the Mup parametrization. When including the impact of faint supernova models in GCE calculations, elemental ratios vary by up to 0.1-0.2 dex in the MW disc; this modification better reproduces observations.

Citation

Pignatari, M., Trueman, T. C., Womack, K. A., Gibson, B. K., Côte, B., Turrini, D., …Lugaro, M. (2023). The chemical evolution of the solar neighbourhood for planet-hosting stars. Monthly notices of the Royal Astronomical Society, 524(4), 6295-6330. https://doi.org/10.1093/mnras/stad2167

Journal Article Type Article
Acceptance Date Jul 14, 2023
Online Publication Date Jul 21, 2023
Publication Date Oct 1, 2023
Deposit Date May 2, 2024
Publicly Available Date May 3, 2024
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 524
Issue 4
Pages 6295-6330
DOI https://doi.org/10.1093/mnras/stad2167
Keywords Stars: abundances; Planetary systems; Solar neighbourhood; Galaxy: abundances; Galaxy: disc; Galaxy: evolution
Public URL https://hull-repository.worktribe.com/output/4377946

Files

Published article (5.9 Mb)
PDF

Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.




You might also like



Downloadable Citations