Brouwers opacity (Eq. (11)) and simple envelope opacity (Eq. (10)) as a function of the distance from the center of the planetary core at an early (solid line) and a late stage (dashed line) in the planet’s growth. We show the Brouwers opacity that arises when the default parameters of Brouwers et al. (2021) are used (v_lim = 2.4 m s⁻¹, F = 0.1), as well as an estimate of the lower limit of the envelope opacity (v_lim = 30.0 m s⁻¹, F = 0). The simple opacity is shown for three different opacity scaling factors κ_env,0. The migration of the planet is suppressed, the growth of the planet initiates at t₀ = 0.1 Myr, and the disk lifetime is 3 Myr. The incoming pebble flux is fixed to 0.6 M_⊕ Myr⁻¹, but can still be lowered by volatile recycling in the planetary envelope. Apart from that, we use our standard parameters (see Table A.2). After 0.2 Myr (3.0 Myr), the planets have a mass of about 0.05 M_⊕ (1.5 M_⊕).