The origin of s-process isotope heterogeneity in the solar protoplanetary disk

Abstract

Rocky asteroids and planets display nucleosynthetic isotope variations that are attributed to the heterogeneous distribution of stardust from different stellar sources in the solar protoplanetary disk. Here we report new high precision palladium isotope data for six iron meteorite groups, which display smaller nucleosynthetic isotope variations than the more refractory neighbouring elements. Based on this observation we present a new model in which thermal destruction of interstellar medium dust results in an enrichment of s-process dominated stardust in regions closer to the Sun. We propose that stardust is depleted in volatile elements due to incomplete condensation of these elements into dust around asymptotic giant branch (AGB) stars. This led to the smaller nucleosynthetic variations for Pd reported here and the lack of such variations for more volatile elements. The smaller magnitude variations measured in heavier refractory elements suggest that material from high-metallicity AGB stars dominated stardust in the Solar System. These stars produce less heavy s-process elements compared to the bulk Solar System composition.

25 pages, 9 figures, 1 table

References in corpus (7)

• Spectroscopic identification of r-process nucleosynthesis in a double neutron star merger
• Evolution of interstellar dust and stardust in the solar neighbourhood
• The s process in massive stars at low metallicity. Effect of primary N14 from fast rotating stars
• Evolution and nucleosynthesis of asymptotic giant branch stellar models of low metallicity
• Rubidium-Rich Asymptotic Giant Branch Stars
• The first stars: CEMP--no stars and signatures of spinstars
• On the need of the Light Elements Primary Process (LEPP)

Cited by in corpus (22)

• Bifurcation of planetary building blocks during Solar System formation
• Terrestrial planet formation from lost inner solar system material
• The s Process and Beyond
• The Mantis Network III: Expanding the limits of chemical searches within ultra hot-Jupiters. New detections of Ca I, V I, Ti I, Cr I, Ni I, Sr II, Ba II, and Tb II in KELT-9 b
• Origin of large meteoritic SiC stardust grains in metal-rich AGB stars
• Growing Mars fast: High-resolution GPU simulations of embryo formation
• The Ni isotopic composition of Ryugu reveals a common accretion region for carbonaceous chondrites
• Cosmic nucleosynthesis: a multi-messenger challenge
• Understanding the evolution and dust formation of carbon stars in the LMC with a look at the JWST
• Thermal processing of primordial pebbles in evolving protoplanetary disks
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• The cosmochemistry of planetary systems
• Infall and Disk Processes - the Message from Meteorites
• Abundances of disk and bulge giants from high-resolution optical spectra V. Molybdenum -- the p-process element
• Representation of s-process abundances for comparison to data from bulk meteorites
• Timescales of Solar System Formation Based on Al-Ti Isotope Correlation by Supernova Ejecta
• Evidence of a primordial isotopic gradient in the inner region of the solar protoplanetary disc
• Nuclear astrophysics
• Interstellar Ices as Carriers of Supernova Material to the Early Solar System
• The NC-CC dichotomy in ruthenium isotopes: Implications for the origin of the late veneer
• Origin of nucleosynthetic isotope variability in the NC reservoir: Evidence from Ti, Cr, and Mo isotopes
• The cosmic journey of dust grains -- from nucleation to planetary system