A perspective from extinct radionuclides on a Young Stellar Object: The Sun and its accretion disk

Abstract

Meteorites, which are remnants of solar system formation, provide a direct glimpse into the dynamics and evolution of a young stellar object (YSO), namely our Sun. Much of our knowledge about the astrophysical context of the birth of the Sun, the chronology of planetary growth from micrometer-sized dust to terrestrial planets, and the activity of the young Sun comes from the study of extinct radionuclides such as 26Al (t1/2 = 0.717 Myr). Here we review how the signatures of extinct radionuclides (short-lived isotopes that were present when the solar system formed and that have now decayed below detection level) in planetary materials influence the current paradigm of solar system formation. Particular attention is given to tying meteorite measurements to remote astronomical observations of YSOs and modeling efforts. Some extinct radionuclides were inherited from the long-term chemical evolution of the Galaxy, others were injected into the solar system by a nearby supernova, and some were produced by particle irradiation from the T-Tauri Sun. The chronology inferred from extinct radionuclides reveals that dust agglomeration to form centimeter-sized particles in the inner part of the disk was very rapid (<50 kyr), planetesimal formation started early and spanned several million years, planetary embryos (possibly like Mars) were formed in a few million years, and terrestrial planets (like Earth) completed their growths several tens of million years after the birth of the Sun.

49 pages, 9 figures, 1 table. Uncorrected preprint

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Cited by in corpus (64)

• Our astrochemical heritage
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• Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk
• Planetary and meteoritic Mg/Si and d30Si variations inherited from solar nebula chemistry
• Astronuclear Physics: a Tale of the Atomic Nuclei in the Skies
• Radioactive nuclei from cosmochronology to habitability
• 60Fe-60Ni chronology of core formation in Mars
• The Mass Budget of Planet Forming Discs: Isolating the Epoch of Planetesimal Formation
• The production of proton-rich isotopes beyond iron: The $\gamma$ process in stars
• Cross Sections for Planetary Systems Interacting with Passing Stars and Binaries
• Stellar origin of the 182Hf cosmochronometer and the presolar history of solar system matter
• The formation of the solar system
• Thermodynamics of Element Volatility and its Application to Planetary Processes
• The Supernova Triggered Formation and Enrichment of Our Solar System
• The $\nu$ process in the light of an improved understanding of supernova neutrino spectra
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• Low 60Fe abundance in Semarkona and Sahara 99555
• Lava Worlds: From Early Earth to Exoplanets
• Bayesian Inference on the Isotopic Building Blocks of Mars and Earth
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• Small Planetesimals in a Massive Disk Formed Mars
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• Geochemical and planetary dynamical views on the origin of Earth's atmosphere and oceans
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• Triggering Collapse of the Presolar Dense Cloud Core and Injecting Short-Lived Radioisotopes with a Shock Wave. III. Rotating Three Dimensional Cloud Cores
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• Stellar energetic particles in the magnetically turbulent habitable zones of TRAPPIST-1-like planetary systems
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• Rocky Planet Formation: Quick and Neat
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• Gas infall via accretion disk feeding Cepheus A HW2
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• Nucleosynthesis of ${}^{92}$Nb and the relevance of the low-lying isomer at 135.5 keV
• Timescales of Solar System Formation Based on Al-Ti Isotope Correlation by Supernova Ejecta
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• Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
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