Under this task a few specific, fully identified, stellar cases are proposed to compare evolution models in order to test the implementation of diffusion in evolution codes. To achieve this a few cases are proposed as the reference:
| CASE | Stellar mass | Y0 | Z0 |
| 3.1 | 1.0 Msun | 0.27 | 0.017 |
| 3.2 | 1.2 Msun | 0.27 | 0.017 |
| 3.3 | 1.3 Msun | 0.27 | 0.017 |
For the comparison, models for each case at different evolutionary stages are required:
| PHASE | Xc | MHe,core |
| A | 0.35 | - |
| B | 0.01 | - |
| C | 0.00 | 0.05 Mstar |
Note: the He core is defined as the region of the star where the Hydrogen abundance X is below 0.01 (as done for Task 1).
The physical assumptions proposed as the reference for the comparison are the same as used for Task 1 and no overhsoot. Regarding diffusion there are no specifications, but a first iteration will focus on diffusion due to pressure, temperature and concentration gradients of
The information and data (to be) available for download are: