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Related Experiment Video

Updated: Jun 7, 2026

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

Stardust silicates from primitive meteorites.

Kazuhide Nagashima¹, Alexander N Krot, Hisayoshi Yurimoto

¹Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Ookayama, Meguro, Tokyo 152-8551, Japan. kazu@geo.titech.ac.jp

|May 1, 2004

Summary

Presolar silicate grains, predating our Solar System, were discovered in primitive meteorites. Their abundance suggests silicates were common in the early Solar System but were likely destroyed by heat.

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Metal-silicate Partitioning at High Pressure and Temperature: Experimental Methods and a Protocol to Suppress Highly Siderophile Element Inclusions

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Published on: June 13, 2015

Scattering And Absorption of Light in Planetary Regoliths

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

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Last Updated: Jun 7, 2026

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

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Published on: June 5, 2014

Metal-silicate Partitioning at High Pressure and Temperature: Experimental Methods and a Protocol to Suppress Highly Siderophile Element Inclusions

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Published on: June 13, 2015

Scattering And Absorption of Light in Planetary Regoliths

Scattering And Absorption of Light in Planetary Regoliths

Published on: July 1, 2019

Area of Science:

Cosmochemistry
Planetary Science
Astronomy

Background:

Primitive chondritic meteorites contain presolar grains, remnants from before our Solar System's formation.
Silicates are expected to be dominant solids in protoplanetary disks, yet presolar silicates have not been found in chondrites.

Purpose of the Study:

To report the in situ discovery of presolar silicate grains in primitive carbonaceous chondrites.
To investigate the origin and abundance of these presolar silicates.

Main Methods:

In situ analysis of presolar silicate grains (0.1-1 microm) within meteorite matrices.
Isotopic analysis of oxygen and silicon in the discovered grains.

Main Results:

Discovery of presolar silicate grains in two primitive carbonaceous chondrites.
Grains show high 17O enrichment (delta17O(SMOW) > 100-400 per thousand) and solar silicon isotopic composition.
Estimated abundance of 3-30 parts per million, higher than other presolar grains but lower than in interplanetary dust particles.

Conclusions:

The presolar silicates likely originated from oxygen-rich red giant or asymptotic giant branch stars.
The lower abundance in meteorites compared to interplanetary dust particles suggests silicate destruction during high-temperature processing in the solar nebula.