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

Open Access

Fig. A.1

Pebble profiles obtained from a two population dust model (Birnstiel et al. 2012, see Appendix A for assumed disk profiles), in comparison with a prediction of the dust surface density Σ_d and Stokes number for largest dust grains (black dashed; Eq. (27)). The classical estimate for St using Eq. (B.1) is also shown in the middle panel (gray dotted).

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