Long-term evolution of the temperature structure in magnetized protoplanetary disks and its implication for the dichotomy of planetary composition

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Table 2

Disk models considered in Sect. 3.

Name	Σ_heat	ϵ_rad	$\bar{α_{ϕ z}}$ $\[\overline{\alpha_{\phi z}}\]$	f_dg
`Fid`	Σ_Am	0.1	Const.	0.01
`Vis`	Σ/2	0.9	Const.	N/A
`eps001`	Σ_Am	0.01	Const.	0.01
`eps1`	Σ_Am	1.0	Const.	0.01
`DG`	Σ_Am	0.1	Const.	0.001
`apz-sgm`	Σ_Am	0.1	Σ-dep	0.01

Notes. The column density for the accretion heating, Σ_heat, was either taken at the midplane (Σ/2) or at the altitude where Am = 0.3 (Σ_Am). The model of $\bar{α_{ϕ z}}$ $\[\overline{\alpha_{\phi z}}\]$ is either a constant value of 10⁻³ (const) or depends on Σ (Σ-dep). The dust-to-gas ratio f_dg was used only for the ionization fraction calculation, while the Rosseland-mean opacity κ in the temperature calculation is given by Eq. (6).

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