(a) Observed abundances (filled circles with error bars) compared with the expected abundances in the secondary star after having captured 90% of the matter ejected within the solid angle subtended by the secondary from a metal‐poor (Z = 0.004) 30 M_⊙ spherically symmetric supernova explosion (M_He = 11 M_⊙) with E_K = 10⁵¹ ergs for two different mass cuts, M_cut = 2.52 M_⊙ (solid line with open circles) and M_cut = 3.04 M_⊙ (dash‐dotted line with open circles). The initial abundances of the secondary star were adopted for the average abundances of the thick‐disk stars with [Fe/H] = −0.7 ± 0.2, and the initial orbital distance was a_c,i ≈ 6 R_⊙. (b) Same as (a), but for a spherically symmetric hypernova explosion (E_K = 20 × 10⁵¹ ergs) for mass cuts of M_cut = 3.04 M_⊙ (solid line with open circles) and M_cut = 4.15 M_⊙ (dash‐dotted line with open circles).