Small-scale and large-scale dynamos in global convection simulations of solar-like stars

Open Access

Table 1.

Summary of runs.

Run	Resolution	Ta[10⁸]	${\bar{Ra}}_{Kram}$ ${\overline{{\text{Ra}}}}_{\mathrm{Kram}}$ [10⁷]	${\bar{Ra}}_{SGS}$ ${\overline{{\text{Ra}}}}_{\mathrm{SGS}}$ [10⁷]	${\tilde{Ra}}_{SGS}$ $\widetilde{{\text{Ra}}}_{\mathrm{SGS}}$	Pr	Re	Co	SLD	Δθ_ν	Δθ_η	Δ_νη
0M	128 × 256 × 128	1.25	73	1.2	48	5.13	27	10.4
0H	128 × 256 × 128	1.25	73	1.2	48	5.13	28	9.9	Yes

1M	256 × 512 × 256	5.00	280	5.9	94	1.52	61	9.3		5°	5°	2
1H	256 × 512 × 256	5.00	280	5.9	94	1.52	66	8.5	Yes

2M	512 × 1024 × 512	20.0	1050	23.7	149	0.58	127	8.9		5°	5°	5
2S	512 × 1024 × 512	20.0	1050	23.7	149	0.58	139	8.1		5°	5°	5
2H	512 × 1024 × 512	20.0	1050	23.7	149	0.58	143	7.9	Yes	5°		5

3M	1024 × 2048 × 1024	80.0	3155	71.5	178	0.27	255	8.9		17°	17°	5
3S	1024 × 2048 × 1024	80.0	3155	71.5	178	0.27	265	8.5		17°	5°	5
3H	1024 × 2048 × 1024	80.0	3155	71.5	178	0.27	287	7.9	Yes	17°		5

4M	2048 × 4096 × 2048	320.0	7536	185.9	184	0.12	517	8.7		17°	5°	5
4M2	2048 × 4096 × 2048	320.0	7536	185.9	184	0.12	549	8.5		17°	5°	5
4S	2048 × 4096 × 2048	320.0	7536	185.9	184	0.12	550	8.2		17°	5°	5

Notes. Columns 2 to 7: input parameters. Columns 8 and 9: solution parameters, calculated from the saturated stage of the simulations. The last four columns indicate whether SLD and/or a diffusion profile in θ was used with the corresponding parameters (see Appendices A and B). All runs had a density contrast Γ_ρ ≡ ⟨ρ⟩_θϕ(0.7R)/⟨ρ⟩_θϕ(R) of roughly 30, and $\tilde{Ω} = 5$ ${\tilde{\Omega}} = 5$ , Pr_SGS = 1. The M and S runs had Pr_M = 1.

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