Hierarchically modelling stars to improve inference of stellar properties with asteroseismology
High-precision asteroseismology has improved estimates of stellar
masses, radii, and ages. However, this has revealed inaccuracies
in typical assumptions regarding properties such as helium
abundance (Y) and the mixing-length theory parameter
(α). We applied a hierarchical Bayesian
model to a sample of main sequence, low-mass dwarf stars to
encode population level information about Y and
α. We showed that our method reduced the
uncertainties in mass, radius and age to 2.5%, 1.2% and 12%
respectively compared to grid-based modelling methods. We also
show that through our new method, uncertainties decrease with
larger sample sizes. With many more asteroseismic targets
expected from PLATO, we expect to further improve our inference
of bulk stellar parameters.