Left: Evolutionary tracks for a sample of stars with m_final = 2.50 M_⊙ at [Fe/H] = −0.15 with varying initial masses and accretion masses, with accretion phases for each model highlighted in blue. Right: Relative surface abundance of the s-process element Ba with log₁₀(Age/yr). The abundance is elevated after the accretion phase, and after the onset of first dredge-up the surface abundance is diluted.