PHysics of Oscillating STars
Published October 22, 2018 | Version v1
Conference paper Open

Model physics in low-mass solar-type stars: atomic diffusion and metallicity mixture

Creators

  • 1. Instituto de Astrof\'{\i}sica e Ci\^{e}ncias do Espa\c{c}o, Universidade do Porto, Rua das Estrelas, PT4150-762 Porto, Portugal
  • 2. School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
  • 3. LESIA, Observatoire de Paris, Universit\'{e} PSL, CNRS, Sorbonne Universit\'{e}, Univ. Paris Diderot, Sorbonne Paris Cit\'{e}, 5 place Jules Janssen, 92195 Meudon, France
  • 4. Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

Description

Using asteroseismic data from the Kepler satellite, we explore the systematic uncertainties arising from changes in the input physics used when constructing evolution models of solar-type stars. We assess the impact of including atomic diffusion and of varying the metallicity mixture on the determination of global stellar parameters (i.e., radius, mass, and age). We find significant systematic uncertainties on global stellar parameters when diffusion is included in stellar grids. Furthermore, we find the systematic uncertainties on the global stellar parameters to be comparable to the statistical uncertainties when a different metallicity mixture is employed in stellar grids.

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Additional details

Related works

Is derived from
Poster: 10.5281/zenodo.1466015 (DOI)
Is identical to
Conference paper: arXiv:1812.00431 (arXiv)
Conference paper: 2018arXiv181200431N (Bibcode)

Funding

PULSATION – Detecting and characterizing exoplanets around evolved stars with NASA's TESS mission 792848
European Commission

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