Exploring the P vs. P relation with flux transport dynamo models of solar-like stars

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Table 1:

Summary of the different cases studied and the values of $R_{\rm e}$ and $C_\Omega$ used in the 2D Babcock-Leighton models.
Case	$\Omega_{0}/\Omega_{\rm S}$	MCKE/10⁴	$v_\theta^{\rm scale}$	$\vec{R}_{\rm e}/10^2$	$\vec{C}_{\Omega}/10^5$
G0.25	0.25	23.4	28.7	20.1	0.351
G0.5	0.5	16.2	23.9	16.7	0.702
G0.6	0.6	12.3	20.9	14.6	0.842
G0.75	0.75	4.75	12.9	9.06	1.05
G0.9	0.9	3.09	10.4	7.29	1.26
G1	1	2.84	10.0	7.00	1.40
G1.25	1.25	2.18	8.76	6.13	1.75
G1.5	1.5	1.98	8.36	5.85	2.11
G1.75	1.75	1.68	7.70	5.39	2.46
G2	2	1.52	7.33	5.13	2.81
G3	3	1.11	6.25	4.38	4.21
G4	4	0.767	5.20	3.64	5.62
G5	5	0.711	5.01	3.51	7.02
G6	6	0.626	4.70	3.29	8.42
G7	7	0.497	4.18	2.93	9.83
G10	10	0.359	3.56	2.49	14.0

The value of $\eta_{\rm t}$ is fixed to $10^{11} ~~ \rm cm^2~s^{-1}$ and the value of s₀ is fixed to $50 ~~ \rm cm~s^{-1}$ . The stellar rotation rate $\Omega _0$ is given in terms of the solar rotation rate $\Omega _{\rm S}$ . $v_\theta^{\rm scale}$ represents the amplitude of $v_\theta$ at the surface at $45^{\circ}$ and is imposed equal to $10 ~~ \rm m~s^{-1}$ for case G1, representing the reference solar mean field dynamo model.

Source LaTeX | All tables | In the text

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