Distributions of the grid modelling results. Left: asteroseismic mass against the normalised core hydrogen mass fraction, . We find the majority of stars to have masses between 1.4 and 1.7 M_⊙ and to be in the first part of their main-sequence evolution with . Note that the -axis is inverted to represent the time evolution from left to right. Right: radius distribution of our sample. We find only a few evolved stars, and most stars have a radius between 1.5 and 2.2 R_⊙, as expected in this mass regime for main-sequence stars.