MESA (r12778) and GYRE (version 6.0) inlist files used in the work described in "Mixed Mode Asteroseismology of Red Giant Stars Through the Luminosity Bump". Published in The Astrophysical Journal, Volume 931, Issue 2, id.116 Two subdirectories are provided in the archive: 1) The directory called "inlists_and_src" contains different MESA inlist files for different evolutionary period (inlist_pms=pre main sequence to beginning of the red giant phase and inlist_rgb=red giant branch through the RGB luminosity bump) of the stellar model. The four subdirectories refer to the four overshooting prescriptions described in the paper. The different inlist files for the different evolutionary states are called by putting their names in the "inlist" file. Two example gyre (version 6.0) inlists are also included in the "inlists" subdirectory. The inlist titled gyre_pi.in calculates the radial, dipole, and quadrupole pi mode frequencies, while the inlist titled gyre.in calculates the non-pi mode frequencies. A custom diffusion cutoff (see Viani et al. 2018, ApJ, 858, 28) are included in the run_star_extras.f file in the "src" subdirectories. There is also a custom subroutine called "other_adjust_mlt_gradT_fraction_overshoot" which is used to change the temperature gradient within the overshooting region for models incorporating full/penetrative overshoot. The subroutine is activated by setting "x_logical_ctrl(1)" to .true. in the MESA inlists. The amplitude of the full overshooting region is controlled with "x_ctrl(1)" 2) The subdirectory named "example_data" include the MESA modelling results used in the paper to produce figure 16, showing the evolution of the gravity mode phase offset through the red giant branch luminosity bump. The GYRE-calculated frequencies are included in the GYRE_OUTPUTS subdirectories. In these models, overshooting from the red giant convective envelope was turned off.

Feel free to email the corresponding author at christopher.lindsay@yale.edu. CJL acknowledges support from a Gruber Science Fellowship. JO acknowledges support from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. SB acknowledges NSF grant AST-2205026.