meteorites; meteors; meteoroids; minor planets; asteroids: general
Abstract :
[en] Context. The origin of the petrologic diversity observed in ordinary chondrites (OCs), the most common meteorites on Earth, remains debated. Competing models invoke either depth-dependent sampling of a single thermally stratified ('onion-shell') parent body or contributions from multiple distinct parent bodies. Aims. We aim to determine which of the two models is preferred for LL chondrites. These are unique among OCs in exhibiting a bimodal petrologic distribution, with most meteorites being LL3 or LL6. Methods. We compared the spectral and mineralogical properties of LL chondrites and corresponding LL-chondrite-like near-Earth objects (NEOs) with their possible sources in the main asteroid belt. We also modelled the thermal histories of the proposed parent bodies, based on revised estimates of parent-body sizes. Results. The spectral and mineralogical diversity of LL chondrites is consistent with contributions from the bright, S-type component of the Nysa family (Nysa_S) and the Flora family, with Nysa_S supplying mainly low-petrologic-type material and Flora supplying higher-grade material. Unequilibrated, LL3 chondrites appear to originate exclusively from Nysa_S. Similarly, LL-chondrite-like NEOs form two distinct subpopulations consistent with origins in these same families. Conclusions. Our results favour multiple parent bodies for LL chondrites. The petrologic differences between the Nysa_S and Flora parent bodies can be explained by differences in their sizes, without requiring different formation times.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Marsset, M.; European Southern Observatory, Germany
Brož, M.; Charles University, Faculty of Mathematics and Physics, Astronomical Institute, V Holešovičkách 2, 18000, Praha, Czech Republic,
Avdellidou, C.; University of Leicester, Department of Physics and Astronomy
Thomas, C. A.; Northern Arizona University
McGraw, L.; Northern Arizona University
Madden-Watson, A.; Northern Arizona University
Minker, K.; Lowell Observatory, Arizona
Monnereau, M.; IRAP, University of Toulouse, CNRS, Toulouse, France,
DeMeo, F. E.; MIT, Department of Earth and Planetary Science
Binzel, R. P.; MIT, Department of Earth and Planetary Science
Mahlke, M.; Université Marie et Louis Pasteur, CNRS, Institut UTINAM (UMR 6213), équipe Astro, 25000, Besançon, France,
Carry, B.; Observatoire de la Cote d'Azur, France
Hanuš, J.; Charles University, Faculty of Mathematics and Physics, Astronomical Institute, V Holešovičkách 2, 18000, Praha, Czech Republic,
Simon, P. N.; Aix-Marseille Universite, Laboratoire d'Astrophysique
Yang, B.; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile, Planetary Science Institute, 1700 E Fort Lowell Rd STE 106, Tucson, AZ, 85719, USA
Beck, P.; Institut de Planétologie et Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, 38000, Grenoble, France
Birlan, M.; Institutul Astronomic al Academiei Române, 5-Cutitul de Argint, Sector 4, 040557, Bucharest, Romania, LTE, Observatoire de Paris, 77 av Denfert Rochereau, 75014, Paris Cedex, France,
Jehin, Emmanuel ; Université de Liège - ULiège > Unités de recherche interfacultaires > Space sciences, Technologies and Astrophysics Research (STAR)
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