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Asteroseismic forward modelling techniques are being used to determinefundamental properties (e.g. mass, radius, and age) of solar-type stars. Theneed to take into account all possible sources of error is of paramountimportance towards a robust determination of stellar properties. We present astudy of 34 solar-type stars for which high signal-to-noise asteroseismic datais available from multi-year Kepler photometry. We explore the internalsystematics on the stellar properties, that is, associated with the uncertaintyin the input physics used to construct the stellar models. In particular, weexplore the systematics arising from: (i) the inclusion of the diffusion ofhelium and heavy elements; and (ii) the uncertainty in solar metallicitymixture. We also assess the systematics arising from (iii) different surfacecorrection methods used in optimisation/fitting procedures. The systematicsarising from comparing results of models with and without diffusion are foundto be 0.5%, 0.8%, 2.1%, and 16% in mean density, radius, mass, and age,respectively. The internal systematics in age are significantly larger than thestatistical uncertainties. We find the internal systematics resulting from theuncertainty in solar metallicity mixture to be 0.7% in mean density, 0.5% inradius, 1.4% in mass, and 6.7% in age. The surface correction method by Sonoiet al. and Ball & Gizon's two-term correction produce the lowest internalsystematics among the different correction methods, namely, ~1%, ~1%, ~2%, and~8% in mean density, radius, mass, and age, respectively. Stellar massesobtained using the surface correction methods by Kjeldsen et al. and Ball &Gizon's one-term correction are systematically higher than those obtained usingfrequency ratios.

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