Post-disruption normalized specific orbital energies of the star-BH system, ε_orb, for a star of mass 1 M_⊙ (left) and 0.5 M_⊙ (right) initially in a parabolic orbit, due to a BH of mass 10 M_⊙ (top) and 40 M_⊙ (bottom), as a function of impact parameter b and MS age (H_c abundance). The dashed line represents parabolic orbits and separates the parameter space into bound (eccentric) and unbound (hyperbolic) orbits. When mass loss is relatively low, a lower value of b generally results in more negative ε_orb in the case of 1 M_⊙ star. This trend continues for the TAMS star. However, for the ZAMS and MAMS stars, significant mass losses can reverse this trend, with hyperbolic orbits also being a possibility (e.g., 1 M_⊙ ZAMS star and 40 M_⊙ BH mass with b < 1.00) 0.5 M_⊙ stars, on the other hand, can become unbound for larger b, with boundedness also depending on the mass of the BH.