SCALING UP ENSEMBLE MODELLING OF GRAVITY-MODE PULSATORS WITH GAIA AND TESS
Abstract
Abstract: Measurements of internal rotation frequencies and chemical mixing efficiencies of (main sequence) gravity mode pulsators have enabled the rigorous testing of the state-of-the-art stellar structure and evolution models. We prepare for future large ensemble modelling of gravity-mode pulsators by relying on a new sample of such stars recently discovered from the 3rd Data Release of the Gaia mission and confirmed by space photometry from TESS. This sample of potential asteroseismic targets is about 23 times larger than the Kepler sample. We use the effective temperature and luminosity inferred from Gaia to deduce evolutionary masses, convective core masses, radii, and ages for ∼14,000 gravity-mode pulsators classified as such from their TESS light curves. We do so by constructing dedicated grids of evolutionary models for rotating stars with input physics from the asteroseismic calibrations of Kepler γ Doradus pulsators. We find the new gravity-mode pulsators to cover an extended observational instability region covering masses from about 1.3 to about 9 M⊙. In this talk, I will provide their mass-luminosity and mass-radius relations, as well as convective core masses. The results suggest that oscillations excited by the opacity mechanism occur uninterruptedly for the mass range above about 2 M⊙, where stars have a radiative envelope aside from thin convection zones in their excitation layers. Furthermore, for a subsample of these stars, we relied on asteroseismic properties of Kepler γ Doradus and slowly pulsating B stars to derive the near-core rotation frequency of the Gaia-discovered pulsators from their dominant prograde dipole gravito-inertial pulsation mode, in addition to the age estimate. I will discuss the evolution of the rotation frequency of ~2,400 stars along the main sequence. A decline of the rotation frequency with a factor of two is seen during the main-sequence evolution for this population of field stars, which covers a mass range from 1.3 to 7 M⊙.