Can We Draw Conclusions on Supernova Shock Wave Propagation Using Short‐Lived Radioactive Isotopes? Article Swipe

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Supernova Physics Neutron star Astrophysics Stars Interstellar medium Isotope Nucleosynthesis Shock wave Astronomy Nuclear physics Galaxy Mechanics

Benjamin Wehmeyer , Andrés Yagüe López , Benoît Côté , Mária Pető , Chiaki Kobayashi , Maria Lugaro ·

YOU? · · 2025 · Open Access · · DOI: https://doi.org/10.1002/asna.70002 · OA: W4410721159

We run a three‐dimensional Galactic chemical evolution (GCE) model to follow the propagation of 53 Mn (exclusively produced from type Ia supernovae, SNIa), 60 Fe (exclusively produced from core‐collapse supernovae, CCSNe), 182 Hf (exclusively produced from intermediate mass stars, IMSs), and 244 Pu (exclusively produced from neutron star mergers, NSMs). By comparing the predictions from our three‐dimensional GCE model to recent detections of 53 Mn, 60 Fe, and 244 Pu on the deep‐sea floor, we draw conclusions about their propagation in the interstellar medium.