Asteroseismic modelling of solar-type stars: internal systematics from input physics and surface correction methods

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DOI

    B. Nsamba, Univ Porto, Universidade do Porto, Dept Fis & Astron, Fac Ciencias, T. L. Campante, Univ Porto, Universidade do Porto, CAUP, Inst Astrofis & Ciencias Espaco, Univ Porto, Universidade do Porto, Dept Fis & Astron, Fac Ciencias, M. J. P. F. G. Monteiro, Univ Porto, Universidade do Porto, Dept Fis & Astron, Fac Ciencias, M. S. Cunha, Univ Porto, Universidade do Porto, Dept Fis & Astron, Fac Ciencias, B. M. Rendle, Univ Birmingham, University of Birmingham, Sch Phys & Astron, D. R. Reese, Univ Paris Diderot, Universite Sorbonne Paris Cite-USPC (ComUE), Sorbonne Universite, Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), University of Paris Diderot, PSL Research University Paris (ComUE), UPMC Univ Paris 06, Sorbonne Univ,LESIA, PSL Res Univ,Sorbonne Paris Cite,CNRS,Observ Pari,
  • K. Verma

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, similar to 1 per cent, similar to 1 per cent, similar to 2 per cent, and similar to 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.

Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Volume477
Issue number4
Pages (from-to)5052-5063
Number of pages12
ISSN0035-8711
DOIs
StatePublished - Jul 2018

    Research areas

  • asteroseismology, stars: evolution, stars: fundamental parameters, stars: oscillations, METAL-POOR STARS, OSCILLATION FREQUENCIES, ELEMENT DIFFUSION, HELIUM ABUNDANCE, SUN, EVOLUTION, HELIOSEISMOLOGY, OPACITIES, INTERIOR, MISSION

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