Gap radius, R_gap, with respect to the accretion rate, ${\dot{M}}_{\star }$, (‘$R_{\text{gap\hspace{0.17em}}}-{\dot{M}}_{\star }$’-wall) for the models from Table 2 that trigger accretion events. The cyan dots represent observational data taken from Ercolano & Pascucci (2017) (labelled as ‘E+2017’). To indicate the possible range of our models, we added two additional models: ‘gap_large’ and ‘gap_small’. The models ‘gap_large’ and ‘gap_small’ have initial accretion rates of ${\dot{M}}_{\text{init\hspace{0.17em}}}=3\times {10}^{-8}{M}_{\odot }{\mathrm{y}\mathrm{r}}^{-1}$ and ${\dot{M}}_{\text{init\hspace{0.17em}}}={10}^{-9}{M}_{\odot }{\mathrm{y}\mathrm{r}}^{-1}$ and X-ray luminosities of 10³⁰ erg s⁻¹ and 10²⁹ erg s⁻¹ were assumed, respectively. These models range from small accretion rates and small gap sizes in the lower-left corner to large gap sizes with accretion rates of ≲3 × 10⁻⁹ M_⊙ yr⁻¹ (lower-right side of the plot).