INTRODUCTION
The extensive grid of massive stellar models has been computed with the open-source code MESA (Paxton et al. 2011, 2013, 2015). It covers the evolutionary phase from the zero-age main sequence until depletion of central hydrogen at the terminal-age main sequence. Different element compositions (in terms of initial hydrogen-mass fraction, Xi, and metallicity, Z) are taken into account. Chemical mixing is included via exponential convective-core overshooting, fov, and diffusive mixing, Dmix, in the radiative envelope. Along the evolutionary tracks, adiabatic frequencies of gravity and pressure modes have been computed with GYRE (Townsend & Teitler, 2013).
The gird is based on the one used by Schmid & Aerts (2016) and uses the following input physics:
- Solar metal mixtures by Asplund et al. (2009)
- OPAL opacity tables (Iglesias & Rogers 1993, 1996)
- Mixing-length theory of convection by Cox and Giuli (1968, chap. 14)
- Schwartzschild instability criterion
- All equilibrium models are nonrotating
Extent of the grid parameters
| begin | end | step | |
| M (M⦿) | 2
12 |
10
20 |
1
2 |
| Xi | 0.68 | 0.72 | 0.02 |
| Z | 0.012 | 0.020 | 0.002 |
| fov | 0.0 | 0.05 | 0.01 |
| log Dmix | 0 | 3 | 1 |
Grid parameters adiabatic pressure modes
| Begin | End | Step / N | |
|---|---|---|---|
| Degree l | 0 | 2 | 1 |
| Radial order n | 0 | 5 | 1 |
| Frequency range (days-1) | 0.05 | 50 | 800 |
Grid parameters adiabatic gravity modes
| Begin | End | Step / N | |
|---|---|---|---|
| Degree l | 0 | 2 | 1 |
| Radial order n | -80 | 0 | 1 |
| Frequency range (days-1) | 0.05 | 8 | 700 |
USE OF THE MODELS
The models are made available to anyone upon request. Due to the large file sizes we cannot provide files for download on this website. We kindly ask users to cite Schmid & Aerts (2016) in any publications in which these models are used and to add the following line to the acknowledgements:
“The computation of the stellar model grid used was funded by the European Community’s Seventh Framework Programme FP7-SPACE-2011-1, project number 312844 (SPACEINN).”
DATA FORMAT
Evolutionary tracks are saved in the MESA format of “history.data”-files. The first line contains column numbers, the second line contains column names, and the third line contains values. The head of each history-file contains global information and initial parameters. Staring from line five, the time dependent parameters are listed. This file explains all column names that are found in the history-file. Additional columns are dP_asym, the asymptotic period spacing in days, and P_asym50, the asymptotic period of the mode with l = 1 and n = -50 in days.
