COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES
© 2016. The American Astronomical Society. All rights reserved. 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...
| Main Authors: | , , , , , , , , |
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| Format: | Article |
| Language: | English |
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American Astronomical Society
2021
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| Online Access: | https://hdl.handle.net/1721.1/137535 |
| _version_ | 1811097716188512256 |
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| author | Vernazza, P. Marsset, M. Beck, P. Binzel, R. P. Birlan, M. Cloutis, E. A. DeMeo, F. E. Dumas, C. Hiroi, T. |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Vernazza, P. Marsset, M. Beck, P. Binzel, R. P. Birlan, M. Cloutis, E. A. DeMeo, F. E. Dumas, C. Hiroi, T. |
| author_sort | Vernazza, P. |
| collection | MIT |
| description | © 2016. The American Astronomical Society. All rights reserved. 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. |
| first_indexed | 2024-09-23T17:03:46Z |
| format | Article |
| id | mit-1721.1/137535 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T17:03:46Z |
| publishDate | 2021 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | mit-1721.1/1375352022-09-29T23:26:22Z COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES Vernazza, P. Marsset, M. Beck, P. Binzel, R. P. Birlan, M. Cloutis, E. A. DeMeo, F. E. Dumas, C. Hiroi, T. Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences © 2016. The American Astronomical Society. All rights reserved. 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. 2021-11-05T16:19:45Z 2021-11-05T16:19:45Z 2016-08 2020-05-05T14:59:03Z Article http://purl.org/eprint/type/JournalArticle 1538-3881 https://hdl.handle.net/1721.1/137535 Vernazza, P., Marsset, M., Beck, P., Binzel, R. P., Birlan, M. et al. 2016. "COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES." Astronomical Journal, 152 (3). en 10.3847/0004-6256/152/3/54 Astronomical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf American Astronomical Society The American Astronomical Society |
| spellingShingle | Vernazza, P. Marsset, M. Beck, P. Binzel, R. P. Birlan, M. Cloutis, E. A. DeMeo, F. E. Dumas, C. Hiroi, T. COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title | COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title_full | COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title_fullStr | COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title_full_unstemmed | COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title_short | COMPOSITIONAL HOMOGENEITY OF CM PARENT BODIES |
| title_sort | compositional homogeneity of cm parent bodies |
| url | https://hdl.handle.net/1721.1/137535 |
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