Radial differential rotation leading to dipole collapse in pre-main-sequence stars

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Table B.1.

Parameters of dipolar initial conditions used in this paper.

Label	Pm	ξ	Ra	Ro_conv	Λ	$f_{dip}^{11}$ $Mathematical equation: $ f^{11}_{\mathrm{dip}} $$	Re	Nu	${Ro}_{sh}^{collapse}$ $Mathematical equation: $ \mathrm{{Ro}}^{\mathrm{collapse}}_{\mathrm{sh}} $$
g ∼ 1/r²
`gr2_1`	4	0.35	2 ⋅ 10⁶	0.044	9.35	0.54	67.9	2.53	0.00425
`gr2_2`	4	0.35	5 ⋅ 10⁶	0.127	29.58	0.67	206.2	7.26	0. 0135
`gr2_3`	4	0.2	1 ⋅ 10⁶	0.025	1.68	0.66	52.6	1.78	0.035
`gr2_4`	4	0.1	5 ⋅ 10⁵	0.015	1.49	0.67	47.7	2.07	0.085
`gr2_5`	6	0.35	1.5 ⋅ 10⁶	0.026	9.75	0.56	42.7	1.82	0.00175
`gr2_6`	6	0.2	1.5 ⋅ 10⁶	0.040	19.93	0.56	94.8	3.75	0.0175
`gr2_7`	6	0.1	5.5 ⋅ 10⁶	0.016	1.49	0.67	47.6	2.07	0.0355

g, Cesam2k20
`gc_1`	4	0.35	1 ⋅ 10⁷	0.084	20.06	0.68	118.5	4.14	0.00875
`gc_2`	4	0.35	1.5 ⋅ 10⁷	0.121	31.42	0.71	171.1	5.78	0.0125

g ∼ r
`gr_1`	4	0.2	8 ⋅ 10⁶	0.029	1.44	0.73	41.8	1.42	0.025
`gr_2`	4	0.2	1.6 ⋅ 10⁷	0.062	15.09	0.74	104.5	2.98	0.25

Notes. The values of all parameters, except the last column, are given for the base case without differential rotation, Ro_sh = 0, and do not change considerably when Ro_sh ≠ 0 (e.g., see Fig. 4). The last column corresponds to the shear Rossby number at the dipole collapse, ${Ro}_{sh}^{collapse}$ $Mathematical equation: $ \mathrm{{Ro}}^{\mathrm{collapse}}_{\mathrm{sh}} $$ , allowing us to reconstruct entire simulation space.

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