2026-05-22 マックス・プランク研究所
Just outside Jupiter’s orbit, a ring-shaped region of high gas pressure formed. In this “dust trap,” over several million years planetesimals of varying compositions were able to form.© MPS / hormesdesign.de
＜関連情報＞
- https://www.mpg.de/26532587/different-meteorites-same-birthplace
- https://iopscience.iop.org/article/10.3847/1538-4357/ae6104
炭素質コンドライトは、圧力上昇域における微惑星形成の後期段階の証拠を提供する Carbonaceous Chondrites Provide Evidence for Late-stage Planetesimal Formation in a Pressure Bump
Nerea Gurrutxaga, Joanna Drążkowska, Vignesh Vaikundaraman, and Thorsten Kleine
The Astrophysical Journal Published: 2026 May 22
DOI:10.3847/1538-4357/ae6104
Abstract
Carbonaceous chondrites are samples from planetesimals that formed 2–4 million years after solar system formation began. They consist of distinct dust components formed at different times and locations in the accretion disk, and whose abundances in carbonaceous chondrites vary over planetesimal formation time. The mechanism that led to this time-varied accretion is not understood, but it is critical for understanding late-stage planetesimal formation. Using a two-dimensional Monte Carlo simulation of dust evolution, we show that differences in dust filtering and delivery rates of distinct dust components to a planet-induced pressure bump in the disk reproduce the observed compositions and formation ages of the carbonaceous chondrites. This implies that carbonaceous chondrites likely formed in a single, long-lived dust trap, most likely outside of Jupiter’s orbit. Because differentiated meteorites, which sample an earlier generation of planetesimals, exhibit similar isotopic variability as the chondrites, they likely have also formed in dust traps, implying these structures were the dominant site for planetesimal formation in the solar system.
