Evolution of the same satellite as in Figure 9 across all the models. First row: Trajectory during their infall into the host halo. Second row: Evolution of the ram pressure (solid line) felt by the gas and the restoring force (dashed line) per unit area. Both lines begin when the satellite comes within $4R_{\mathrm{vir}}^{\mathrm{host}}$ and P_rest is defined as long as the satellite contain gas. Third row: Evolution of the ratio of ram pressure to the restoring force per unit area. Gray horizontal dashed line marks P_ram/P_rest = 1. Fourth row: Comparison between the tidal and ram pressure radius, represented as dashed and solid lines, respectively. Fifth row: Ratio between E_s and E_int to identify high velocity satellite-satellite encounter. Red horizontal dashed line marks the threshold $log\left(E_{\mathrm{s}}/E_{\mathrm{int}}\right)>-1.5$. Sixth row: Evolution of the star-forming gas mass, defined as gas with n_H>1 cm⁻³ and a temperature below 10⁴ K. Seventh row: Evolution of the ratio M_gas/M_halo, the 1% is marked as a red dashed line for reference. Eighth row: SFR evolution, usually named Star Formation History (SFH). Ninth row: Evolution of the stellar mass. Stellar mass loss serves as an effective tracer for tidal stripping in the ISM. Tenth row: Mass inflow rate evolution for studying the effect of strangulation. Gray background lines in rows six to ten represent the evolution of the same parameter for field galaxies with M_peak>10¹⁰ M_⊙ for each model. The time domain where snapshots are still not available for each specific code are indicated as a gray shaded region. Vertical dashed lines mark the pericenter passages for each model. The same plot for a sample of (intercode matched) satellite galaxies can be found at this link, where examples of galaxies of different masses and following more radial or more tangential orbits are provided.