Under this task a few specific, fully identified, stellar cases are proposed to compare evolution models. The comparison has to consider the physics used in the calculation in order to allow for a detailed comparison of the results and by how much the numerical implementation of the physics may affect the result from different codes. The comparison should also be done between pairs of model builders.
| CASE | Stellar mass | Y0 | Z0 | Central X | Central T | Mass He core | Overshoot | Comment |
| 1.1 | 0.9 Msun | 0.28 | 0.02 | 0.35 | - | - | - | MS |
| 1.2 | 1.2 Msun | 0.28 | 0.02 | 0.69 | - | - | - | ZAMS |
| 1.3 | 1.2 Msun | 0.26 | 0.01 | - | - | 0.1 Msun | - | Post-MS |
| 1.4 | 2.0 Msun | 0.28 | 0.02 | - | 1.9x107 | - | - | Pre-MS |
| 1.5 | 2.0 Msun | 0.26 | 0.02 | 0.01 | - | - | 0.15 Hp | TAMS |
| 1.6 | 3.0 Msun | 0.28 | 0.01 | 0.69 | - | - | - | ZAMS |
| 1.7 | 5.0 Msun | 0.28 | 0.02 | 0.35 | - | - | - | MS |
The physical assumptions proposed as the reference for the comparison are given below. These can (and should) be changed for each particular case as some fine tuning of the physics may be required.
| ITEM | Selection | References |
| EoS | OPAL | Rogers et al. (1996, 2001 Tables) |
| Opacities | OPAL | Iglesias & Rogers (1996) + Alexander & Fergusson (1994) |
| Reaction rates | NACRE | Angulo et al. (1999) |
| Convection | MLT (α = 1.6) | Böhm-Vitense (1958) + Henyey et al. (1965) |
| Overshoot | ∇=∇ad | Zahn (1991) + ... |
| Diffusion/settling | - none - | - |
| Mixture | Solar | Grevesse & Noels (1993) |
| Atmosphere | Gray | - |
The information and data available for download are: