Disk enrichment mass-fraction as function of the distance to the supernova and its angle with respect to the proto-planetary disk’s rotation axis for SN11aof (left) and SN10a (right). The colored contours give the amount of accreted mass from the supernova remnant as a fraction of the mass of the surviving disk (scale to the right). The enclosed and shaded regions are as in Fig. 11. The small top-left area of the hashed region which overlaps with an enrichment of at least m_shell ∕M_disk ≳ 10⁻³ satisfies all the criteria of the model. The absence of a hashed region in the left panel indicates that there is no consistent solution across all requirements in our simulations for SN10a.