Calibrating angular momentum transport in intermediate-mass stars from gravity-mode asteroseismology II. Modelling 2937 BAF-type stars

Grids of rotating MESA (r24.03.1) models used in Mombarg & Mathis (2026). The angular momentum transport is done fully diffusively where the effective viscosity, nu, is either taken constant (10^6, 10^7, 10^8 cm^2/s) or computed from the prescription for the Tayler-Spruit dynamo (TS) in MESA. The grids contain the following information:

M:                       mass in Msun
omega_i:            initial rotation ZAMS as a fraction of the initial Kepler critical rotation frequency
fov:                     near-core boundary mixing (overshoot) parameter for exponential overshoot
Z:                        metallicity (all 0.014)
Xc/X:                   hydrogen-mass fraction in core over the initial hydrogen-mass fraction
age_Myr:            age in Myr
mcc:                   mass of convective core in Msun
Pi0:                     buoyancy travel time in seconds
Omega_cpd:      near-core rotation frequency in cycles per day
log_L:                 log luminosity (Lsun)
Teff:                    effective temperature in Kelvin
log_g:                 log surface gravity (cgs)
omega_current: current fraction of critical rotation
log_R:                 log radius
Omega_surf:     current surface rotation frequency in rad/sec
n14_surf:            nitrogen-14 surface mass fraction
o16_surf:            oxygen-16 surface mass fraction
c12_surf:            carbon-12 surface mass fraction
h1_surf:              hydrogen-1 surface mass fraction

Example to read in the files with Python:

import pickle as pkl

with open('.../grid_Gaia_Z0.014_nu*.pkl', 'rb') as handle:
    grid = pkl.load(handle)