Refractory solid condensation detected in an embedded protoplanetary disk

• 成果类型: Article
• 署名作者: McClure, M. K.; Van't Hoff, Merel; Francis, Logan; Bergin, Edwin; Rocha, Will R. M.; Sturm, J. A.; Harsono, Daniel; van Dishoeck, Ewine F.; Black, John H.; Noble, J. A.; Qasim, D.; Dartois, E.
• 署名单位: Leiden University - Excl LUMC; Leiden University; University of Michigan System; University of Michigan; Purdue University System; Purdue University; Leiden University - Excl LUMC; Leiden University; National Tsing Hua University; Chalmers University of Technology; Aix-Marseille Universite; Centre National de la Recherche Scientifique (CNRS); CNRS - Institute for Engineering & Systems Sciences (INSIS); Southwest Research Institute; Centre National de la Recherche Scientifique (CNRS); Universite Paris Saclay
• 刊物名称: Nature
• ISSN/ISSBN: 0028-2968
• DOI: 10.1038/s41586-025-09163-z
• 发表日期: 2025-07-17
• 关键词: silicate; spectroscopy; accretion; emission; models; GROWTH

摘要

Terrestrial planets and small bodies in our Solar System are theorized to have assembled from interstellar solids mixed with rocky solids that precipitated from a hot, cooling gas1,2. The first high-temperature minerals to recondense from this gaseous reservoir start the clock on planet formation3,4. However, the production mechanism of this initial hot gas and its importance to planet formation in other systems are unclear. Here we report the astronomical detection of this t = 0 moment, capturing the building blocks of a new planetary system beginning its assembly. The young protostar HOPS-315 is observed at infrared and millimetre wavelengths with the James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA), revealing a reservoir of warm silicon monoxide gas and crystalline silicate minerals low in the atmosphere of a disk within 2.2 au of the star, physically isolated from the millimetre SiO jet. Comparison with condensation models with rapid grain growth and disk structure models suggests the formation of refractory solids analogous to those in our Solar System. Our results indicate that the environment in the inner disk region is influenced by sublimation of interstellar solids and subsequent refractory solid recondensation from this gas reservoir on timescales comparable with refractory condensation in our own Solar System.