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Compositional homogeneity of CM parent bodies.

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dc.contributor.author Vernazza, P.
dc.contributor.author Marsset, M.
dc.contributor.author Beck, P.
dc.contributor.author Binzel, R. P.
dc.contributor.author Birlan, M.
dc.contributor.author Cloutis, E. A.
dc.contributor.author DeMeo, F. E.
dc.contributor.author Dumas, C.
dc.contributor.author Hiroi, T.
dc.date.accessioned 2018-03-05T16:50:57Z
dc.date.available 2018-03-05T16:50:57Z
dc.date.issued 2016-08-10
dc.identifier.citation Vernazza, P., M. Marsset, P. Beck, R.P. Binzel, M. Birlan, E.A. Cloutis, F.E. DeMeo, C. Dumas, and T. Hiroi. "Compositional homogeneity of CM parent bodies." Astronomical Journal 152 (3) (2016): 54 (10 pp). DOI: 10.3847/0004-6256/152/3/54. en_US
dc.identifier.issn 0004-6256
dc.identifier.uri http://hdl.handle.net/10680/1381
dc.description.abstract CM chondrites are the most common type of hydrated meteorites, making up ∼1.5% of all falls. Whereas most CM chondrites experienced only low-temperature (∼0°C–120°C) aqueous alteration, the existence of a small fraction of CM chondrites that suffered both hydration and heating complicates our understanding of the early thermal evolution of the CM parent body(ies). Here, we provide new constraints on the collisional and thermal history of CM-like bodies from a comparison between newly acquired spectral measurements of main-belt Ch/Cgh-type asteroids (70 objects) and existing laboratory spectral measurements of CM chondrites. It first appears that the spectral variation observed among CM-like bodies is essentially due to variations in the average regolith grain size. Second, the spectral properties of the vast majority (unheated) of CM chondrites resemble both the surfaces and the interiors of CM-like bodies, implying a “low” temperature (<300°C) thermal evolution of the CM parent body (ies). It follows that an impact origin is the likely explanation for the existence of heated CM chondrites. Finally, similarly to S-type asteroids and (2) Pallas, the surfaces of large (D > 100 km)—supposedly primordial—Ch/ Cgh-type main-belt asteroids likely expose the interiors of the primordial CM parent bodies, a possible consequence of impacts by small asteroids (D < 10 km) in the early solar system. en_US
dc.description.sponsorship The MIT component of this work is supported by NASA grant 09-NEOO009-0001, and by the National Science Foundation under grants Nos. 0506716 and 0907766. F.E.D. acknowledges support from NASA under grant No. NNX12AL26G issued through the Planetary Astronomy Program. E.A.C. thanks the Canada Foundation for Innovation, the Manitoba Research Innovations Fund, the Canadian Space Agency, the University of Winnipeg, and the Natural Sciences and Engineering Research Council of Canada for supporting the establishment and operation of the University of Winnipeg's Planetary Spectrophotometer Facility and this study.
dc.description.uri http://iopscience.iop.org/article/10.3847/0004-6256/152/3/54/meta
dc.language.iso en en_US
dc.publisher The Astronomical Journal en_US
dc.subject meteorites, meteors, meteoroids – methods: data analysis – methods: laboratory: solid state – methods: observational – minor planets, asteroids: general – techniques: spectroscopic en_US
dc.title Compositional homogeneity of CM parent bodies. en_US
dc.type Article en_US
dc.identifier.doi 10.3847/0004-6256/152/3/54


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