^1,2Noun, M. et al. (>10)
Life 9, 44 Link to Article [DOI: 10.3390/life9020044]
¹Institut de Physique Nucléaire d’Orsay, UMR 8608, CNRS/IN2P3, Université Paris-Sud, Université Paris-Saclay, Orsay, F-91406, France
²Lebanese Atomic Energy Commission, NCSR, Beirut, 11-8281, Lebanon

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^1,2Neveu, M.,³Vernazza, P.
Astronophysical Journal 875, 30 Link to Article [DOI: 10.3847/1538-4357/ab0d87]
¹University of Maryland, 4296 Stadium Dr., College Park, MD 20742, United States
²NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20770, United States
³Aix-Marseille Universite, CNRS, Laboratoire d’Astrophysique de Marseille, 38 Rue Frederic Joliot Curie, Marseille, F-13013, France

The parent bodies of ordinary chondrites, carbonaceous CM chondrites, and interplanetary dust particles (IDPs) represent most of the mass of the solar system’s small (D ≤ 250 km) bodies. The times of formation of the ordinary and carbonaceous CM chondrite parent bodies have previously been pinpointed, respectively, to ≈2 and 3–4 million years after calcium–aluminum-rich inclusions (CAIs). However, the timing of the formation of IDP parent bodies such as P- and D-type main-belt asteroids and Jupiter Trojans has not been tightly constrained. Here, we show that they formed later than 5–6 million years after CAIs. We use models of their thermal and structural evolution to show that their anhydrous surface composition would otherwise have been lost due to melting and ice-rock differentiation driven by heating from the short-lived radionuclide ²⁶Al. This suggests that IDP-like volatile-rich small bodies may have formed after the gas of the protoplanetary disk dissipated and thus later than the massive cores of the giant planets. It also confirms an intuitive increase in formation times with increased heliocentric distance, and suggests that there may have been a gap in time between the formation of carbonaceous chondrite (chondrule-rich) and IDP (chondrule-poor) parent bodies.

^1,2Guitreau, M.,³Flahaut, J.
Nature Communications 10, 2457 Link to Article [DOI: 10.1038/s41467-019-10382-y]
¹School of Earth and Environmental Sciences, University of Manchester, Oxford road, Manchester, M13 9PL, United Kingdom
²Université Clermont Auvergne, Laboratoire Magmas et Volcans, 6 avenue Blaise Pascal, Aubière, 63178, France
³CRPG, CNRS/Université de Lorraine, Vandœuvre-lès-Nancy, 54500, France

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^1,2Smith, K.E.,²House, C.H.,³Arevalo, R.D., Jr.,^4,5Dworkin, J.P.,^1,4,5Callahan, M.P.
Nature Communications 10, 2777 Link to Article [DOI: 10.1038/s41467-019-10866-x]
¹Department of Chemistry and Biochemistry, Boise State University, Boise, ID 83725, United States
²Department of Geosciences and Penn State Astrobiology Research Center, Pennsylvania State University, University Park, PA 16801, United States
³Department of Geology, University of Maryland, College Park, MD 20742, United States
⁴Goddard Center for Astrobiology, NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States
⁵Astrochemistry Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States

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