Nucleosynthetic yields of intermediate-mass primordial to extremely metal-poor stars

Context. Stellar models and nucleosynthetic yields of primordial to extremely metal-poor (EMP) stars are crucial interpret the surface abundances most observed and, ultimately, better understand earliest stellar populations. In addition, they key ingredients Galactic chemical evolution models. Aims. We aim characterise fates, determine updated intermediate-mass between EMP metallicity ( Z = 10 −10 , −8 −7 −6 −5 ). also probed uncertainties in nucleosynthesis oldest stars, namely those related treatment convection convective boundaries wind prescriptions during asymptotic giant branch (AGB) phase. Methods. analyse from their main sequence, through thermally pulsing AGB (TP-AGB), latest stages evolution, using Monash-Mount Stromlo code MONSTAR . The results were post-processed with MONSOON which allowed for determination 77 species up 62 Ni. By comparing them similar calculations existing literature, we inspected effects input physics on Results. From evolutionary point view, as reported former works, identified proton ingestion episodes (PIEs) our lowest-mass lowest-metallicity Models a narrow initial mass range around 5 M ⊙ experience cessation thermal pulses, final fates type-I1/2 supernovae cannot be discarded. However, eventually leading formation electron-capture is considerably reduced compared works. All ≳6–7 corrosive second dredge-up analogously experiencing PIEs, undergo significant metal enrichment envelopes. associated increase opacities allows develop solar-like TP-AGB or TP-super-AGB, ultimately becoming white dwarfs. Except undergoing all show signatures both efficient third hot-bottom burning, activation NeNa cycle MgAlSi chains. This leads creation vast amounts CNO, typical [N/Fe] > 4), characteristic abundance signature [C/Fe] [O/Fe]. Our present dramatic differences respect recent literature metallicities. reason these discrepancies lay poorly known winds above all, boundaries.