2025/01/24 by Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara +1 · 1 voice · 1 citation
Physics and Astronomy · Biochemistry, Genetics and Molecular Biology · Earth and Planetary Sciences · #Astro and Planetary Science #Geomagnetism and Paleomagnetism Studies #Geology and Paleoclimatology Research
paper · doi:10.3847/2041-8213/ada554
openalex created_date 2025/01/01 · openalex publication_date 2025/01/24 · openalex updated_date 2026/07/31
Abstract The radioactive decay of short-lived 26 Al– 26 Mg has been used to estimate the timescales over which 26 Al was produced in a nearby star and the protosolar disk evolved. The chronology commonly assumes that 26 Al was uniformly distributed in the protosolar disk; however, this assumption is challenged by the discordance between the timescales defined by the Al–Mg and assumption-free Pb–Pb chronometers. We find that the 26 Al heterogeneity is correlated with the nucleosynthetic stable Ti isotope variation, which can be ascribed to the nonuniform distribution of ejecta from a core-collapse supernova in the disk. We use the Al–Ti isotope correlation to calibrate variable 26 Al abundances in Al–Mg dating of early solar system processes. The calibrated Al–Mg chronometer indicates a ≥1 Myr gap between parent body accretion ages of carbonaceous and noncarbonaceous chondrites. We further use the Al–Ti isotope correlation to constrain the timing and location of the supernova explosion, indicating that the explosion occurred at 20–30 pc from the protosolar cloud, 0.94 +0.25/–0.21 Myr before the formation of the oldest solar system solids. Our results imply that the Sun was born in association with a ∼25 M ʘ star.