Disk fraction in the remnant galaxy (f_{disk,+1 Gyr}) as a function of $⟨{\theta }_{{\mathbf{L}}_{\text{main}},{\mathbf{L}}_{\text{orbit}}}^{\mathrm{\prime }}⟩,⟨{\theta }_{{\mathbf{L}}_{\text{sat}},{\mathbf{L}}_{\text{orbit}}}^{\mathrm{\prime }}⟩$, and ⟨θ_{r, v}⟩ for the mergers with mass ratio over 1/2. The dots in panels a and b are colored with f_{disk,+1 Gyr}. The dashed lines in panel a denote θ_sum=30°, 60°, 90°, 120°, and 150° from the bottom-left to the top-right. Panels c and d illustrate two extreme cases result in high and low disk fractions in the remnant galaxy. In panel c, both the main progenitor galaxy and the satellite galaxy are aligned parallel to the merger orbital plane, and their orbital configuration is spiral-in, leading to a high disk fraction in the remnant galaxy. In panel d, both the main progenitor galaxy and the satellite galaxy are aligned perpendicular to the merger orbital plane and with a head-on orbit, resulting in a very low disk fraction in the remnant galaxy. For the two typical scenarios represented by panels c and panel d, two samples are selected for display in Appendix C. These two samples are indicated in panel b by a blue star in the upper left corner and a red star in the lower right corner.