Paper X
"Stellar evolution with rotation:
X. Wolf-Rayet star populations at solar metallicity"
Georges Meynet & André Maeder (2003)
Paper XI
"Stellar evolution with rotation:
XI. Wolf-Rayet star populations at different metallicity"
Georges Meynet & André Maeder (2005)
In this directory, you will find the tracks corresponding to Paper X, and in that one, the tracks corresponding to Paper XI.
There are two types of files:
In the files beginning with a "D" all the data for a given model are given on one line. These files are useful for plotting the data.
In the files beginning with a "T" all the data for a given model are given on three lines. These files are useful for printing the data.
The names of the different files give information on the data it contains:
The initial mass is indicated after the D or T (120 Msol=c2).
The metallicity is indicated after the z, 20 meaning a mass fraction of heavy element equal to 0.020 (solar metallicity)
After the letter S, a zero means that the initial axial rotational velocity on the ZAMS is 0 km/s at the equator; 3 means that the initial axial rotational velocity on the ZAMS is 300 km/s at the equator. The corresponding average values of the velocities during the Main sequence is between 180 and 240 km/s (see paper X) well in the observed range of the average velocities measured for these type of stars. The letter A after the 3 means that the wind anisotropies have been taken into account.
Each track is described by 350 points well chosen in order to:
- allow interpolation between models with the same number; typically models with equal number have during the Main Sequence approximately the same value of the mass fraction of hydrogen at the centre;
- well describe the shape of the track.
Meaning of the columns in the files D....
| 1 | model number | |
| 2 | age | (in years) |
| 3 | mass | (in Msol) |
| 4 | Log L/Lsol | |
| 5 | Log Teff | |
| 6 | surface abundance of | 1H (in mass fraction) |
| 7 | " | 4He |
| 8 | " | 12C |
| 9 | " | 13C |
| 10 | " | 14N |
| 11 | " | 16O |
| 12 | " | 17O |
| 13 | " | 18O |
| 14 | " | 20Ne |
| 15 | " | 22Ne |
| 16 | mass of convective core | (fraction of total mass |
| 17 | Log Teff | not corrected for optical thickness of the wind (WR only) |
| 18 | Log(mass loss rate) | (in Msol per year) |
| 19 | Log rho at the center | |
| 20 | Log Tc | |
| 21 | central abundance of | 1H (in mass fraction) |
| 22 | " | 4He |
| 23 | " | 12C |
| 24 | " | 13C |
| 25 | " | 14N |
| 26 | " | 16O |
| 27 | " | 17O |
| 28 | " | 18O |
| 29 | " | 20Ne |
| 30 | " | 22Ne |
| 31 | R(pole)/R(equat.) | |
| 32 | equatorial velocity | (in km/sec) |
| 33 | Omega/Omega(critical) |
Meaning of the columns in the files T....
first line:
| 1 | model number | |
| 2 | age | (in years) |
| 3 | mass | (in Msol) |
| 4 | Log L/Lsol | |
| 5 | Log Teff | |
| 6 | surface abundance of | 1H (in mass fraction) |
| 7 | " | 4He |
| 8 | " | 12C |
| 9 | " | 13C |
| 10 | " | 14N |
| 11 | " | 16O |
| 12 | " | 17O |
| 13 | " | 18O |
| 14 | " | 20Ne |
| 15 | " | 22Ne |
second line:
| 1 | mass of convective core | (fraction of total mass |
| 2 | Log Teff | not corrected for optical thickness of the wind (WR only) |
| 3 | Log(mass loss rate) | (in Msol per year) |
| 4 | Log rho at the center | |
| 5 | Log Tc | |
| 6 | central abundance of | 1H (in mass fraction) |
| 7 | " | 4He |
| 8 | " | 12C |
| 9 | " | 13C |
| 10 | " | 14N |
| 11 | " | 16O |
| 12 | " | 17O |
| 13 | " | 18O |
| 14 | " | 20Ne |
| 15 | " | 22Ne |
third line:
| 1 | R(pole)/R(equat.) | |
| 2 | equatorial velocity | (in km/sec) |
| 3 | Omega/Omega(critical) |
For further informations or suggestions, please send an email to Georges Meynet
