2018/07/03 by D. Vescovi, M. Busso, S. Palmerini +8
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Asymptotic giant branch #Formation and evolution of the Solar System #Galaxy #Neutron star #Nucleosynthesis #Solar System #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/aad191
published as ApJ 863, 115 (2018) · Accepted for publication on ApJ
arxiv created 2018/07/03 · openalex created_date 2018/07/10 · openalex publication_date 2018/08/16 · arxiv updated 2018/08/21 · openalex updated_date 2026/08/06
Abstract Recent improvements in stellar models for intermediate-mass stars and massive stars (MSs) are recalled, together with their expectations for the synthesis of radioactive nuclei of lifetimes τ ≲ 25 Myr, in order to re-examine the origins of now extinct radioactivities that were alive in the solar nebula. The Galactic inheritance broadly explains most of them, especially if r -process nuclei are produced by neutron star merging, according to recent models. Instead, 26 Al, 41 Ca, 135 Cs, and possibly 60 Fe require nucleosynthetic events close to the solar formation. We outline the persisting difficulties to account for these nuclei by intermediate-mass stars (2 ≲ M / M ⊙ ≲ 7–8). Models of their final stages now predict the ubiquitous formation of a 13 C reservoir as a neutron capture source; hence, even in the presence of 26 Al production from deep mixing or hot bottom burning, the ratio 26 Al/ 107 Pd remains incompatible with measured data, with a large excess in 107 Pd. This is shown for two recent approaches to deep mixing. Even a late contamination by an MS encounters problems. In fact, the inhomogeneous addition of supernova debris predicts nonmeasured excesses on stable isotopes. Revisions invoking specific low-mass supernovae and/or the sequential contamination of the presolar molecular cloud might be affected by similar problems, although our conclusions here are weakened by our schematic approach to the addition of SN ejecta. The limited parameter space that remains to be explored for solving this puzzle is discussed.