Left: survival map of a star in the (i_in,ini, X) plane for a fiducial EMRI configuration motivated by the typical orbital scale of GSN 069. The color indicates the maximum inner orbital eccentricity ﹩{e}_{{\rm{in}},{\rm{\max }}}﹩ reached during the SA evolution, including octupole-order terms and 1PN relativistic apsidal precession. The calculation uses M_• = 4 × 10⁵ M_⊙, a_in = 300 M_•, e_in,ini = 0.01, and a circular outer orbit with e_out = 0. For each displayed point, the plotted value is the largest ﹩{e}_{{\rm{in}},{\rm{\max }}}﹩ obtained after sampling a logarithmic grid of tertiary SMBH masses 10⁵ ≤ M_e/M_⊙ ≤ 10⁶ and eight initial values of ω_in, subject to the hierarchy cut a_out/a_in ≥ 2.8. The black solid contour denotes the TDE boundary ﹩{a}_{{\rm{in}}}(1-{e}_{{\rm{in}},{\rm{\max }}})={r}_{{\rm{TDE}}}﹩, and the red dashed contour denotes ﹩{e}_{{\rm{in}},{\rm{\max }}}=0.04﹩. Regions enclosed by the TDE boundary would tidally disrupt a solar-type star and are therefore disfavored if the observed QPE source contains a surviving star. Right: same as the left panel, but with a much lower initial inner orbital eccentricity e_in,ini = 10⁻⁵. The yellow shaded regions in both panels denote the TDE regime obtained from a rescan of the same (M_e, a_out) grid with a_in,ini = 600M_• and GW dissipation.