Change in the orbital period ΔP (in days) for remnants in pTDEs of main sequence stars with mass of M_⋆ = 1, 2, and 3 M_⊙ in hydrodynamics simulations, as a function of the fractional mass loss ΔM/M_⋆. The original stars are Solar metallicity main sequence stars with a core hydrogen mass fraction of X_H ≃ 0.01 (Terminal age: solid lines) and 0.3 (Middle age: dashed lines). The simulations suggest that ΔP in severe pTDEs of terminal-age main-sequence stars can be compatible with the change in T_recur between cycles 1 and 2 (≃ − 70 days, grey horizontal line) of J0456-20.