Supernova Propagation And Cloud Enrichment: A new model for the origin of ${}^{60}$Fe in the early solar system

Abstract

The radioactive isotope ${}^{60}$Fe ($T_{1/2}=1.5$ Myr) was present in the early solar system. It is unlikely that it was injected directly into the nascent solar system by a single, nearby supernova. It is proposed instead that it was inherited during the molecular cloud stage from several supernovae belonging to previous episodes of star formation. The expected abundance of ${}^{60}$Fe in star forming regions is estimated taking into account the stochasticity of the star-forming process, and it is showed that many molecular clouds are expected to contain ${}^{60}$Fe (and possibly ${}^{26}$Al [$T_{1/2}=0.74$ Myr]) at a level compatible with that of the nascent solar system. Therefore, no special explanation is needed to account for our solar system's formation.

15 pages, 3 figures

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Cited by in corpus (13)

• A perspective from extinct radionuclides on a Young Stellar Object: The Sun and its accretion disk
• Solar system genealogy revealed by extinct short-lived radionuclides in meteorites
• Tidal Limits to Planetary Habitability
• Feedback in Clouds II: UV Photoionisation and the first supernova in a massive cloud
• The formation of the solar system
• Distributions of Short-Lived Radioactive Nuclei Produced by Young Embedded Stellar Clusters
• Light Element Nucleosynthesis in a Molecular Cloud Interacting with a Supernova Remnant and the Origin of Beryllium-10 in the Protosolar Nebula
• Supernova enrichment of planetary systems in low-mass star clusters
• Chemical enrichment of the pre-solar cloud by supernova dust grains
• Distribution and kinematics of 26Al in the Galactic disc
• Insights on the Sun birth environment in the context of star-cluster formation in hub-filament systems
• The Astrophysical Environment of the Solar Birthplace
• An upper limit for the growth of inner planets?