Notes. The different geometries are illustrated in Fig. 1. Model names in the paper are suffixed with Warm or Cold depending on whether the radius fit R_p(Ṁ, M_p) to cold-accreting or warm-accreting planets (see Sect. 3.2) is used. ^(a)Fraction of the planet’s surface covered by the accretion flow. ^(b)Opening angles of the accretion cone covering each pole (Eq. (1)); for illustration. ^(c)Starting position of the infalling gas with a radial velocity v_r = 0 there. ^(d)Outer limit of the optical radiative transfer calculation, limited to r_max ≈ 100 R_p due to uncertainty in the structure of the far layers. The exact value is however inconsequential for SpherAcc and Polar.