Structural evolution during the most extreme mass-loss case in our simulations (r_p/r_t = 1.2, ﹩{M}_{{\rm{core}}}=10\,{M}_{\oplus }﹩). Upper panel: density slices showing the planet before and after tidal encounters. The postencounter remnant is visibly distorted and spinning, with a significant portion of the envelope stripped. Lower left: quantitative comparison of the spherically averaged density profiles before (solid line) and after (dotted–dashed line) the encounter, which provides a good fit over most of the radial extent. Lower right: cumulative mass profile comparison, showing that over 75% of the remnant’s mass is enclosed within 1 R_J. The good agreement between the pre-encounter and postencounter profiles over most of the radial extent justifies our approach of treating each encounter independently, with the remnant relaxed back to a spherical configuration.