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Dust from supernovae and their progenitors in the solar nebula

Nature Astronomy volume 6, pages 1027–1034 (2022)Cite this article

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Abstract

Pristine stardust grains from the interstellar gas and dust cloud from which our Solar System formed some 4.57 billion years ago are present in small quantities in primitive Solar System materials, such as certain types of meteorite, interplanetary dust particles and cometary matter. As these grains are older than our Solar System, they are known as presolar grains. They can be recognized because they carry large isotopic abundance anomalies that are the result of nucleosynthetic processes in their parent stars, namely, asymptotic giant branch stars, supergiants, supernovae and novae. From astronomical observations and dust-evolution models, it is still not clear to what extent various stellar sources, especially supernovae, contributed dust to the interstellar medium. Since the discovery of presolar grains more than 30 years ago, supernova grains have been considered to be only a minor subpopulation of presolar grains, with relative contributions of ∼10% for silicates, the most abundant type of presolar stardust grains. Recently conducted studies of presolar grains with improved analysis techniques have changed this view considerably, and suggest that supernovae and their progenitors contributed substantially to the dust inventory of the solar nebula, namely, >30% for silicates and >25% in total if other stardust minerals are considered. Here we review the recent findings from studies of presolar grains and discuss implications for future presolar grain studies, interstellar dust models and the interpretation of astronomical observations of dust in supernova ejecta.

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Fig. 1: Chemically separated, micrometre-sized presolar grains from supernova explosions placed on gold foils.
Fig. 2: Abundances of presolar (stardust) grains in the matrix of primitive meteorites.
Fig. 3: NanoSIMS ion images of Mg, Al and Si isotopes and Mg isotopic ratios of a presolar silicate grain.
Fig. 4: Magnesium isotopic systematics of presolar silicate grains.
Fig. 5: C and N isotopic compositions of presolar SiC grains, and their most likely stellar sources.

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Acknowledgements

We thank the participants of the online workshop ‘Supernovae and Interstellar Dust’, organized by NORDITA on 12–14 April 2021, for inspiring this Review. This work was supported by the Max Planck Society.

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  1. Max Planck Institute for Chemistry, Mainz, Germany

    Peter Hoppe, Jan Leitner, János Kodolányi & Stephan Borrmann

  2. Institute for Atmospheric Physics, Johannes Gutenberg University Mainz, Mainz, Germany

    Stephan Borrmann

  3. Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, Orsay, France

    Anthony P. Jones

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All authors meet the journal’s authorship criteria and participated in the discussion and design of the manuscript. P.H. wrote most of the manuscript and coordinated co-author contributions. A.P.J. contributed to the writing of the section on astronomical observations and models. J.L., J.K., S.B. and A.P.J. reviewed and substantially revised the manuscript.

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Hoppe, P., Leitner, J., Kodolányi, J. et al. Dust from supernovae and their progenitors in the solar nebula. Nat Astron 6, 1027–1034 (2022). https://doi.org/10.1038/s41550-022-01737-5

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