Table 1.
Overview of our two-dimensional simulations of a 3.5 M⊙ star.
| Name | Grid | 1D Model | fov | MCZ, i | Mmixed, i | Int. | dt | Mixing rate | Rib | tmax | tmax/τconv |
|---|---|---|---|---|---|---|---|---|---|---|---|
| H3.5 | 10242 | ∇ex | 0 | 0.69 | 0.69 | RK | U | 4.0 ⋅ 10−6 | 627 | 2 ⋅ 108 | 340 |
| M3.5 | 5122 | ∇ex | 0 | 0.69 | 0.69 | RK | U | 6.5 ⋅ 10−6 | 592 | 1 ⋅ 108 | 200 |
| E3.5 | 20482 | ∇ex | 0 | 0.69 | 0.69 | RK | U | 1.0 ⋅ 10−5 | 3031 | 1 ⋅ 107 | 20 |
| H3.5-pc | 10242 | ∇ex | 0 | 0.69 | 0.69 | PC | U | 6.0 ⋅ 10−6 | 2141 | 6 ⋅ 107 | 100 |
| H3.5-igw | 10242 | ∇ex | 0 | 0.69 | 0.69 | PC | IGW | 1.3 ⋅ 10−5 | 766 | 1 ⋅ 107 | 20 |
| H3.5-T | 10242 | T | 0 | 0.69 | 0.69 | PC | U | 4.2 ⋅ 10−6 | 1771 | 2 ⋅ 108 | 430 |
| H3.5-ov1.0 | 10242 | ∇ex | 0.01 | 0.72 | 0.83 | RK | U | 2.5 ⋅ 10−6 | 936 | 8 ⋅ 107 | 140 |
| H3.5-ov1.7 | 10242 | ∇ex | 0.017 | 0.78 | 1.00 | RK | U | 1.5 ⋅ 10−7 | 1193 | 3 ⋅ 107 | 50 |
| H3.5-ov2.0 | 10242 | ∇ex | 0.02 | 0.78 | 1.02 | RK | U | 6.4 ⋅ 10−8 | 1580 | 7 ⋅ 107 | 130 |
| H3.5-ov3.0 | 10242 | ∇ex | 0.03 | 0.78 | 1.14 | RK | U | 2.5 ⋅ 10−16 | 2236 | 4 ⋅ 107 | 70 |
Notes. The model name, which is given in the first column, indicates the grid size of the simulation (M: medium; H: high; E: extremely high), which is listed in the second column. It also indicates the mass of the star in solar units (3.5). The model name of simulations which differ otherwise from the reference model H3.5 includes further characters (see text). The third column gives the quantity that is kept identical in the two-dimensional model to that in the one-dimensional one (see Sect. 2.3). The fourth column gives the overshooting parameter used in the one-dimensional stellar evolution calculations. The mass (in solar units) of the initial CZ and that of the homogeneously mixed core can be found in columns five and six, respectively. The seventh column shows the time integration method, the timestep being calculated according to the criterion given in column eight (see text for details). The ninth and tenth column give the time-averaged mixing rates for t > 107 s in units of M⊙ yr−1 and the bulk Richardson number Rib of the convective boundary, respectively. The last two columns show the final physical time and the number of convective turnovers covered by the simulation.
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