Table 2.
Stellar parameter for models used in the main simulations (see Sect. 4) in this investigation.
| Model | K/1012 cm2 s−1 | ν/1012 cm2 s−1 | Re | Average vrms/104 cm s−1 | MLT velocity/104 cm s−1 |
|---|---|---|---|---|---|
| 3 M⊙ midMs | 5 | 4 | 483 | 10.5 | 0.69 ± 0.18 |
| 5 M⊙ midMs | 5 | 5 | 832 | 14.2 | 1.2 ± 0.19 |
| 7 M⊙ midMs | 5 | 5 | 1658 | 21.0 | 1.8 ± 0.42 |
| 10 M⊙ midMs | 5 | 5 | 2559 | 23.6 | 2.4 ± 0.43 |
| 13 M⊙ midMs | 5 | 5 | 3932 | 28.2 | 3.0 ± 0.9 |
Notes. The average vrms is the root-mean-square of the total velocity in the horizontal direction averaged over the radial extent of the convection zone and the time domain given in Fig. 4. The value, K, is a multiplication factor, which is used to in Eq. (10) to set the thermal diffusivity in our simulations. The viscosity, ν is a constant value throughout the stellar model. Since stellar density varies up to six orders of magnitude, from roughly 101 g cm−1 to 10−5 g cm−1 within the models (see Fig. 1), the thermal diffusion varies up to three orders of magnitude (from Eq. (10)), and thus, the Prandtl number, 
, varies up to three orders of magnitude.
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