Stellar model grid for massive stars (D5.8)


The extensive grid of massive stellar models has been computed with the open-source code MESA (Paxton et al. 201120132015). 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:

Extent of the grid parameters

  begin end step
M (M⦿) 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


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).”


Evolutionary tracks are saved in the MESA format of “”-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 = 1 and = -50 in days.

Exploitation of Space Data for Innovative Helio- and Asteroseismology