Relative importance of convective uncertainties in massive stars

Author:

Kaiser Etienne A12ORCID,Hirschi Raphael123,Arnett W David4,Georgy Cyril5,Scott Laura J A1ORCID,Cristini Andrea16ORCID

Affiliation:

1. Astrophysics Group, Keele University, Keele, Staffordshire ST5 5BG, UK

2. NuGrid Collaboration, https://www.nugridstars.org

3. Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan

4. Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA

5. Department of Astronomy, University of Geneva, Ch. Maillettes 51, CH-1290 Versoix, Switzerland

6. Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA

Abstract

ABSTRACT In this work, we investigate the impact of uncertainties due to convective boundary mixing (CBM), commonly called ‘overshoot’, namely the boundary location and the amount of mixing at the convective boundary, on stellar structure and evolution. For this we calculated two grids of stellar evolution models with the MESA code, each with the Ledoux and the Schwarzschild boundary criterion, and vary the amount of CBM. We calculate each grid with the initial masses of 15, 20, and $25\, \rm {M}_\odot$. We present the stellar structure of the models during the hydrogen and helium burning phases. In the latter, we examine the impact on the nucleosynthesis. We find a broadening of the main sequence with more CBM, which is more in agreement with observations. Furthermore, during the core hydrogen burning phase there is a convergence of the convective boundary location due to CBM. The uncertainties of the intermediate convective zone remove this convergence. The behaviour of this convective zone strongly affects the surface evolution of the model, i.e. how fast it evolves redwards. The amount of CBM impacts the size of the convective cores and the nucleosynthesis, e.g. the 12C to 16O ratio and the weak s-process. Lastly, we determine the uncertainty that the range of parameter values investigated introduces and we find differences of up to $70{{\ \rm per\ cent}}$ for the core masses and the total mass of the star.

Funder

European Cooperation in Science and Technology

National Science Foundation

H2020 European Research Council

European Commission

Horizon 2020 Framework Programme

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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