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000364050 037__ $$aGSI-2026-00232
000364050 041__ $$aEnglish
000364050 1001_ $$0P:(DE-Ds200)OR3007$$aThielemann, Friedrich-Karl$$b0$$ugsi
000364050 1112_ $$aVLT, SUPERNOVAE, BRUNO$$cGarching$$d2025-01-07 - 2025-01-11$$wGermany
000364050 245__ $$aClues on the (supernovae or non-supernovae) Origins of the Elements from Galactic Archeology
000364050 260__ $$c2025
000364050 3367_ $$033$$2EndNote$$aConference Paper
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000364050 520__ $$aLow-metallicity stars are witnesses of the first stellar nucleosynthesis events in the Galaxy, as their surface abundances reflect the composition of the interstellar medium from which they were born. Aside from the primordial Big Bang nucleosynthesis, massive stars, due to their short lifetimes, dominate the wind and explosive ejecta into the interstellar medium of the early Galaxy. Most of them will end as core-collapse supernova (CCSN) explosions, and typical abundance patterns reflect their influence. Essentially all CCSNe eject Fe (decaying from radioactive 56Ni). Therefore, it is interesting to test whether other elements found in low-metallicity stars are correlated with Fe, i.e. whether they have been co-produced in the contributing sources or require either different or additional astrophysical origins. We concentrate in our analysis on stars with [Fe/H]
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000364050 773__ $$a10.5281/ZENODO.15765631
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000364050 9101_ $$0I:(DE-Ds200)20121206GSI$$6P:(DE-Ds200)OR3007$$aGSI Helmholtzzentrum für Schwerionenforschung GmbH$$b0$$kGSI
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000364050 9141_ $$y2025
000364050 9201_ $$0I:(DE-Ds200)KNA-20160901OR396$$kKNA$$lNukleare Astrophysik & Struktur$$x0
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