Notes. ^aStellar parameters M_⋆, R_⋆ and L_⋆ are taken from pre-main sequence (PMS) isochrones created by Baraffe et al. (2015) for a T Tauri star with an age of t = 1 Myr. ^bThe rotation period P_⋆ is chosen to lie in the expected range between 1 and 10 days (e.g. Irwin & Bouvier 2009). ^cB_⋆ for Class II objects is believed to lie between 0.1 kG and 1.0 kG (e.g. Johnstone et al. 2014). ^dX-ray luminosities of classical T Tauri stars lie between 10²⁸ erg s⁻¹ and 10³² erg s⁻¹ (e.g. Preibisch et al. 2005). ^eAccretion rates for classical T Tauri stars lie between 10⁻¹⁰ M_⊙ yr⁻¹ and 10⁻⁷ M_⊙ yr⁻¹ (see Vorobyov et al. 2017). ^fViscosity due to MRI is believed to result in α between 10⁻⁴ and 10⁻¹ (e.g. Zhu et al. 2007; Vorobyov & Basu 2009). ^gAD reduces the effectivity of MRI, which results in a smaller α_AD (e.g. Delage et al. 2022). ^hThe base viscosity is much lower than the viscosity caused by MRI; hence α_base ≪ α_MRI. ⁱA plasma beta, β₀(r_out), in our reference model corresponds to B_∞ ≈ 3.8 ⋅ 10⁻³ G. This is in the range of [10⁻⁵ G, 10⁻¹ G] from studies of the fossil field in protostellar cores (e.g. Crutcher et al. 2004; Masson et al. 2016).