Complementary figures for paper 'The ESO UVES/FEROS Large Programs of TESS OB pulsators II. On the physical origin of macroturbulence'

<p>These are figures from Appendices C and D of the paper <strong>'The ESO UVES/FEROS Large Programs of TESS OB pulsators II. On the physical origin of macroturbulence' (Serebriakova et al. Accepted on 17 Oct 2024 for publication in A&amp;A)</strong>. Appendices C and D are moved to Zenodo following the request of the editor. The figures demonstrate MESA model properties used to compare with observed macroturbulent velocities in massive stars. Appendix C focuses on emphasising the role of opacity bumps and subsurface convection throughout evolution. Appendix D explores wave propagation in these models.</p> <p><strong>Appendix C: MESA internal profiles</strong>. Each figure contains a grid of model internal profiles of stellar properties computed with MESA. Initial mass varies in rows: 60, 20, 12, 7, and 3 Solar masses. In columns, three evolutionary stages are presented: MS, TAMS, and Hertzsprung gap. Models in Fig.1-4 were computed with Solar metallicity Z=0.014, and in Fig. 5-8 - with LMC metallicity Z=0.006. Fig. 1,5 - opacity and convective velocity VS temperature, Fig. 2,6 - opacity and convective velocity VS radius(zoomed), Fig. 3,7 - opacity and convective velocity VS radius(full), Fig. 4,8 - Sign of squared Brunt-V&auml;is&auml;l&auml; frequency and convective velocity as a fraction of sound speed VS radius. See the paper for details.&nbsp;</p> <p><strong>Appendix D: Propagation diagrams</strong>. Each figure contains a grid of propagation diagrams (shaded with g-modes and p-modes cavities) computed for the same models as before. Fig. 3 and 6 are complemented with tunnelling frequency omega_min - see 'Section 5: On wave tunnelling through subsurface convective layers' &nbsp;for details with examples in Fig. 8 of the paper. &nbsp;</p> <p>&nbsp;</p>