2018/04/13 by Benard Nsamba, B. Nsamba, T. L. Campante +6 · 58 citations
Physics and Astronomy · #Adaptive optics and wavefront sensing #Asteroseismology #Astronomy and Astrophysical Research #Astrophysics #Metallicity #Photometry (optics) #Physics #RADIUS #Stars #Stellar, planetary, and galactic studies #Systematics #astro-ph.SR
paper · pdf · doi:10.1093/mnras/sty948
published in Monthly Notices of the Royal Astronomical Society 477(4), 5052-5063 (Oxford University Press) · 13 pages, 10 figures, 4 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society Journal
arxiv created 2018/04/13 · openalex publication_date 2018/04/16 · arxiv updated 2018/05/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Asteroseismic forward modelling techniques are being used to determine fundamental properties (e.g. mass, radius, and age) of solar-type stars. The need to take into account all possible sources of error is of paramount importance towards a robust determination of stellar properties. We present a study of 34 solar-type stars for which high signal-to-noise asteroseismic data are available from multiyear Kepler photometry. We explore the internal systematics on the stellar properties, that is associated with the uncertainty in the input physics used to construct the stellar models. In particular, we explore the systematics arising from (i) the inclusion of the diffusion of helium and heavy elements; (ii) the uncertainty in solar metallicity mixture; and (iii) different surface correction methods used in optimization/fitting procedures. The systematics arising from comparing results of models with and without diffusion are found to be 0.5 per cent, 0.8 per cent, 2.1 per cent, and 16 per cent in mean density, radius, mass, and age, respectively. The internal systematics in age are significantly larger than the statistical uncertainties. We find the internal systematics resulting from the uncertainty in solar metallicity mixture to be 0.7 per cent in mean density, 0.5 per cent in radius, 1.4 per cent in mass, and 6.7 per cent in age. The surface correction method by Sonoi et al. and Ball & Gizon’s two-term correction produce the lowest internal systematics among the different correction methods, namely, ∼1 per cent, ∼1 per cent, ∼2 per cent, and ∼8 per cent in mean density, radius, mass, and age, respectively. Stellar masses obtained using the surface correction methods by Kjeldsen et al. and Ball & Gizon’s one-term correction are systematically higher than those obtained using frequency ratios.