2021/11/18 by Marco Fatuzzo, M. Fatuzzo, Fred C. Adams +1
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Diffusion #Isotope #Molecular cloud #Nuclear physics #Nuclear physics research studies #Physics #Population #Radiogenic nuclide #Solar System #Star formation #Stars #Supernova #Thermodynamics #astro-ph.EP #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/ac38a7
accepted for publication in ApJ
arxiv created 2021/11/18 · openalex publication_date 2022/01/01 · arxiv updated 2022/02/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Short-lived radioactive nuclei (half-life τ 1/2 ∼ 1 Myr) influence the formation of stars and planetary systems by providing sources of heating and ionization. Whereas many previous studies have focused on the possible nuclear enrichment of our own solar system, the goal of this paper is to estimate the distributions of short-lived radionuclides (SLRs) for the entire population of stars forming within a molecular cloud. Here we focus on the nuclear species 60 Fe and 26 Al, which have the largest impact due to their relatively high abundances. We construct molecular-cloud models and include nuclear contributions from both supernovae and stellar winds. The resulting distributions of SLRs are time dependent with widths of ∼3 orders of magnitude and mass fractions ρ SLR / ρ * ∼ 10 −11 –10 −8 . Over the range of scenarios explored herein, the SLR distributions show only modest variations with the choice of cloud structure (fractal dimension), star formation history, and cluster distribution. The most important variation arises from the diffusion length scale for the transport of SLRs within the cloud. The expected SLR distributions are wide enough to include values inferred for the abundances in our solar system, although most of the stars are predicted to have smaller enrichment levels. In addition, the ratio of 60 Fe/ 26 Al is predicted to be greater than unity, on average, in contrast to solar system results. One explanation for this finding is the presence of an additional source for the 26 Al isotope.