The importance of the dynamical corotation torque for the migration of low-mass planets - 1D analytical prescriptions verified by 2D hydrodynamical simulations

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Table 1

Summary of initial parameters explored in 2D hydrody-namic simulations presented in Section 3.2 (Q₀: Toomre-Q parameter at the planet’s initial orbital radius; α_vis: turbulent alpha viscosity, β = –d log Σ₀ / d log r).

Q₀	α_vis	β	Grid’s radial spacing
8	{10^–3, 10^–4, 10^–5}	${\frac{1}{2}, 1}$ $\left\{ {{1 \over 2},\,1} \right\}$	Linear
	{10^–3, 10^–4, 10^–5}	${\frac{3}{2}, 2}$ $\left\{ {{3 \over 2},\,2} \right\}$	Logarithmic
12	{10^–4, 10^–5}	${\frac{1}{2}, 1}$ $\left\{ {{1 \over 2},\,1} \right\}$	Linear
16	{10^–4, 10^–5}	${\frac{1}{2}, 1}$ $\left\{ {{1 \over 2},\,1} \right\}$	Linear
24	{10^–4, 10^–5}	${\frac{1}{2}, 1}$ $\left\{ {{1 \over 2},\,1} \right\}$	Linear
32	{10^–4, 10^–5}	${\frac{1}{2}, 1}$ $\left\{ {{1 \over 2},\,1} \right\}$	Linear

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