Evidence for an asteroid–comet continuum from simulations of carbonaceous microxenolith dynamical evolution |
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| Authors: | Giacomo BRIANI Alessandro MORBIDELLI Matthieu GOUNELLE David NESVORNÝ |
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| Institution: | 1. Dipartimento di Fisica e Astronomia, Università di Firenze, Largo E. Fermi 2, 50125 Firenze, Italy;2. Laboratoire de Minéralogie et Cosmochimie du Muséum, UMR7202, Muséum National d’Histoire Naturelle – CNRS, 61 rue Buffon, 75005 Paris, France;3. Present address: Laboratoire Interuniversitaire des Systèmes Atmosphériques, UMR 7583 du CNRS, Universités Paris 7 et 12, Créteil, France;4. Département Cassiopée, UMR6202, Observatoire de la C?te d’Azur – CNRS, 06304 Nice Cedex 4, France;5. Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, Colorado 80302, USA |
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| Abstract: | Abstract– Micrometeoroids with 100 and 200 μm size dominate the zodiacal cloud dust. Such samples can be studied as micrometeorites, after their passage through the Earth atmosphere, or as microxenoliths, i.e., submillimetric meteorite inclusions. Microxenoliths are samples of the zodiacal cloud dust present in the asteroid Main Belt hundreds of millions years ago. Carbonaceous microxenoliths represent the majority of observed microxenoliths. They have been studied in detail in howardites and H chondrites. We investigate the role of carbonaceous asteroids and Jupiter‐family comets as carbonaceous microxenolith parent bodies. The probability of low velocity collisions of asteroidal and cometary micrometeoroids with selected asteroids is computed, starting from the micrometeoroid steady‐state orbital distributions obtained by dynamical simulations. We selected possible parent bodies of howardites (Vesta) and H chondrites (Hebe, Flora, Eunomia, Koronis, Maria) as target asteroids. Estimates of the asteroidal and cometary micrometeoroid mass between 2 and 4 AU from the Sun are used to compute the micrometeoroid mass influx on each target. The results show that all the target asteroids (except Koronis) receive the same amount (within the uncertainties) of asteroidal and cometary micrometeoroids. Therefore, both these populations should be observed among howardite and H chondrite carbonaceous microxenoliths. However, this is not the case: carbonaceous microxenoliths show differences similar to those existing among different groups of carbonaceous chondrites (e.g., CI, CM, CR) but two sharply distinct populations are not observed. Our results and the observations can be reconciled assuming the existence of a continuum of mineralogical and chemical properties between carbonaceous asteroids and comets. |
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